183 results on '"Francisco J. Castander"'
Search Results
2. A machine learning approach to galaxy properties: Joint redshift - stellar mass probability distributions with Random Forest.
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S. Mucesh, William G. Hartley, Antonella Palmese, Ofer Lahav, L. Whiteway, A. Amon, Keith C. Bechtol, Gary M. Bernstein, Aurelio Carnero Rosell, Matias Carrasco Kind, A. Choi, K. Eckert, S. Everett, Daniel Gruen, Robert A. Gruendl, I. Harrison, E. M. Huff, Nikolay Kuropatkin, Ignacio Sevilla-Noarbe, Erin Sheldon, Brian Yanny, Michel Aguena, Sahar Allam, D. Bacon, Emmanuel Bertin, S. Bhargava, D. Brooks, Jorge Carretero, Francisco J. Castander, Christopher J. Conselice, Matteo Costanzi, Martín Crocce, Luiz Nicolaci da Costa, M. E. S. Pereira, J. DeVicente, Shantanu Desai, H. Thomas Diehl, Alex Drlica-Wagner, August E. Evrard, I. Ferrero, Brenna L. Flaugher, Pablo Fosalba, Joshua A. Frieman, Juan García-Bellido, Enrique Gaztañaga, David W. Gerdes, Julia Gschwend, G. Gutierrez, Samuel R. Hinton, Devon L. Hollowood, Klaus Honscheid, David J. James, K. Kuehn, Marcos Lima, H. Lin, Marcio A. G. Maia, Peter Melchior, Felipe Menanteau, Ramon Miquel, Robert Morgan, Francisco Paz-Chinchón, Andreas Alejandro Plazas, Eusebio Sánchez, Victor E. Scarpine, Michael S. Schubnell, Santiago Serrano, M. Smith, Eric Suchyta, Gregory G. Tarlé, D. Thomas, C. To, T. N. Varga, and R. D. Wilkinson
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- 2020
3. CosmoHub: Interactive exploration and distribution of astronomical data on Hadoop.
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Pau Tallada, Jorge Carretero, Jordi Casals, Carles Acosta-Silva, Santiago Serrano, Marc Caubet, Francisco J. Castander, Eduardo César, Martín Crocce, Manuel Delfino, Martin Eriksen, Pablo Fosalba, Enrique Gaztañaga, Gonzalo Merino, Christian Neissner, and Nadia Tonello
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- 2020
4. DES science portal: Computing photometric redshifts.
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Julia Gschwend, A. Carnero Rossel, Ricardo Ogando, Angelo Fausti Neto, Marcio A. G. Maia, Luiz Nicolaci da Costa, Marcos Lima, Paulo S. S. Pellegrini, Riccardo Campisano, C. Singulani, C. Adean, Christophe O. Benoist, Michel Aguena, Matias Carrasco Kind, Tamara M. Davis, J. DeVicente, William G. Hartley, Ben Hoyle, Antonella Palmese, Iftach H. Sadeh, Timothy M. C. Abbott, Filipe B. Abdalla, Sahar Allam, James Annis, Jacobo Asorey, David D. Brooks, Josh Calcino, Daniela Carollo, Francisco J. Castander, Chris D'Andrea, Shantanu Desai, August E. Evrard, Pablo Fosalba, Joshua A. Frieman, Juan García-Bellido, Karl Glazebrook, David W. Gerdes, Robert A. Gruendl, Gaston R. Gutiérrez, Samuel R. Hinton, Devon L. Hollowood, Klaus Honscheid, Janie K. Hoormann, David J. James, Kyler W. Kuehn, Nikolay Kuropatkin, Ofer Lahav, Geraint F. Lewis, Christopher E. Lidman, Huan Lin, Edward MacAulay, Jennifer L. Marshall, Peter Melchior, Ramon Miquel, Anais Möller, Andreas Alejandro Plazas, Eusebio Sánchez, Basillio X. Santiago, Victor E. Scarpine, Rafe H. Schindler, Ignacio Sevilla-Noarbe, Mathew C. Smith, Natalia E. Sommer, Eric Suchyta, Mollye E. C. Swanson, Gregory G. Tarlé, Brad E. Tucker, Douglas L. Tucker, Syed Ashraf Uddin, and Alistair R. Walker
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- 2018
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5. The PAU survey: measurements of the 4000 Å spectral break with narrow-band photometry
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Pablo Renard, Malgorzata Siudek, Martin B Eriksen, Laura Cabayol, Zheng Cai, Jorge Carretero, Ricard Casas, Francisco J Castander, Enrique Fernandez, Juan García-Bellido, Enrique Gaztanaga, Henk Hoekstra, Benjamin Joachimi, Ramon Miquel, David Navarro-Girones, Cristóbal Padilla, Eusebio Sanchez, Santiago Serrano, Pau Tallada-Crespí, Juan De Vicente, Anna Wittje, Angus H Wright, Ministerio de Economía y Competitividad (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, European Commission, Generalitat de Catalunya, ETH Zurich, National Natural Science Foundation of China, Leiden University, Netherlands Organization for Scientific Research, National Science Centre (Poland), and Ministerio de Educación y Ciencia (España)
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,FOS: Physical sciences ,Galaxies: evolution ,Astronomy and Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The D4000 spectral break index is one of the most important features in the visible spectrum, as it is a proxy for stellar ages and is also used in galaxy classification. However, its direct measurement has always been reserved to spectroscopy. Here, we present a general method to directly measure the D4000 with narrow-band (NB) photometry; it has been validated using realistic simulations, and then evaluated with PAUS NBs, cross-matched with VIPERS spectra (iAB < 22.5, 0.562 < z < 0.967). We also reconstruct the D4000 with the SED-fitting code CIGALE; the use of PAUS NBs instead of broad-bands significantly improves the SED fitting results. For D4000n, the direct measurement has ⟨SNR⟩∼4, but we find that for iAB < 21 all direct D4000 measurements have SNR>3. The CIGALE D4000n has ⟨SNR⟩∼20, but underestimates the error by >50 per cent. Furthermore, the direct method recreates well the D4000–SFR relation, as well as the D4000–mass relation for blue galaxies (for red galaxies, selection effects impact the results). On the other hand, CIGALE accurately classifies galaxies into red and blue populations. We conclude that the direct measurement of D4000 with narrow-band photometry is a promising tool to determine average properties of galaxy samples, with results compatible with spectroscopy., The PAU Survey is partially supported by the Spanish Ministry of Economy and Competitiveness (MINECO) under grants CSD2007-00060, AYA2015-71825, ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, MDM-2015-0509 and Juan de la Cierva fellowship and Latin American Chinese European Galaxy Formation Network (LACEGAL) and Enabling Weak Lensing Cosmology (EWC) Marie Sklodowska-Curie grant No 734374 and No 776247 with European Research Development Fund (ERDF) funds from the EU Horizon 2020 Programme, some of which include ERDF funds from the European Union. IEEC and IFAE are partially funded by the Institució Centres de Recerca de Catalunya (CERCA) and Beatriu de Pinos program of the Generalitat de Catalunya. Funding for PAUS has also been provided by Durham University (via the European Research Council (ERC) StG DEGAS-259586), ETH Zurich, Leiden University (via ERC StG ADULT-279396 and Netherlands Organisation for Scientific Research (NWO) Vici grant 639.043.512), University College London and from the European Union’s Horizon 2020 research and innovation programme under the grant agreement No 776247 EWC. The PAU data center is hosted by the Port d’Informació Científica (PIC), maintained through a collaboration of CIEMAT and IFAE, with additional support from Universitat Autònoma de Barcelona and ERDF. We acknowledge the PIC services department team for their support and fruitful discussions. PR and ZC are supported by National Science Foundation of China (grant No. 12073014). The results published have been funded by the European Union’s Horizon 2020 research and innovation programme under the Maria Sklodowska-Curie (grant agreement No. 754510), the National Science Centre of Poland (grant UMO-2016/23/N/ST9/02963) and by the Spanish Ministry of Science and Innovation through Juan de la Cierva-formacion program (reference FJC2018-038792-I). AHW is supported by an ERC Consolidator Grant (No. 770935).
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- 2022
6. Accurate dark matter halo elongation from weak-lensing stacking analysis
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Elizabeth J Gonzalez, Kai Hoffmann, Enrique Gaztañaga, Diego R García Lambas, Pablo Fosalba, Martin Crocce, Francisco J Castander, Martín Makler, European Commission, Agencia Nacional de Promoción Científica y Tecnológica (Argentina), Consejo Nacional de Investigaciones Científicas y Técnicas (Argentina), Universidad Nacional de Córdoba (Argentina), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), and Fundação de Amparo à Pesquisa do Estado de São Paulo
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Space and Planetary Science ,Gravitational lensing: weak ,Dark matter ,FOS: Physical sciences ,Astronomy and Astrophysics ,Galaxies: clusters: general ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Shape estimates that quantifying the halo anisotropic mass distribution are valuable parameters that provide information on their assembly process and evolution. Measurements of the mean shape estimates for a sample of cluster-sized haloes can be used to test halo formation scenarios, as well as improving the modelling of potential biases in constraining cosmological parameters using these systems. In this work, we test the recovery of halo cluster shapes and masses applying weak-lensing stacking techniques. To this end, we use lensing shear and a new dark-matter halo catalogue, derived from the light-cone output of the cosmological simulation MICE-GC. We perform this study by combining the lensing signals obtained for several samples of haloes, selected according to their mass and redshift, taking into account the main directions of the dark-matter distributions. In the analysis, we test the impact of several potential introduced systematics, such as the adopted modelling, the contribution of the neighbouring mass distribution, miscentring, and misalignment effects. Our results show that when some considerations regarding the halo relaxation state are taken into account, the lensing semi-axial ratio estimates are in agreement within a 5 per cent with the mean shapes of the projected dark-matter particle distribution of the stacked haloes. The presented methodology provides a useful tool to derive reliable shapes of galaxy clusters and to contrast them with those expected from numerical simulations. Furthermore, our proposed modelling, that takes into account the contribution of neighbouring haloes, allows to constraint the elongation of the surrounding mass distribution., This project has received funding from the European Union’s Horizon 2020 – Research and Innovation Framework Programme under the Marie Sklodowska-Curie Actions grant agreement No 734374. This work was also partially supported by Agencia Nacional de Promoción Científica y Tecnológica (PICT-2020-SERIEA-01404), the Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET, Argentina), and the Secretaría de Ciencia y Tecnología de la Universidad Nacional de Córdoba (SeCyT-UNC, Argentina). This work has made use of CosmoHub. CosmoHub has been developed by the Port d’Informació Científica (PIC), maintained through a collaboration of the Institut de Física d’Altes Energies (IFAE) and the Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), and was partially funded by the ‘Plan Estatal de Investigación Científica y Técnica y de Innovación’ program of the Spanish government. MM is partially supported by FAPERJ and CNPq.
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- 2022
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7. The PAU survey: Measurement of narrow-band galaxy properties with approximate bayesian computation
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Luca Tortorelli, Malgorzata Siudek, Beatrice Moser, Tomasz Kacprzak, Pascale Berner, Alexandre Refregier, Adam Amara, Juan García-Bellido, Laura Cabayol, Jorge Carretero, Francisco J. Castander, Juan De Vicente, Martin Eriksen, Enrique Fernandez, Enrique Gaztanaga, Hendrik Hildebrandt, Benjamin Joachimi, Ramon Miquel, Ignacio Sevilla-Noarbe, Cristóbal Padilla, Pablo Renard, Eusebio Sanchez, Santiago Serrano, Pau Tallada-Crespí, and Angus H. Wright
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galaxy evolution ,galaxy surveys ,010308 nuclear & particles physics ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,010303 astronomy & astrophysics ,01 natural sciences ,Astrophysics::Galaxy Astrophysics - Abstract
Narrow-band imaging surveys allow the study of the spectral characteristics of galaxies without the need of performing their spectroscopic follow-up. In this work, we forward-model the Physics of the Accelerating Universe Survey (PAUS) narrow-band data. The aim is to improve the constraints on the spectral coefficients used to create the galaxy spectral energy distributions (SED) of the galaxy population model in Tortorelli et al. 2020. In that work, the model parameters were inferred from the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) data using Approximate Bayesian Computation (ABC). This led to stringent constraints on the B-band galaxy luminosity function parameters, but left the spectral coefficients only broadly constrained. To address that, we perform an ABC inference using CFHTLS and PAUS data. This is the first time our approach combining forward-modelling and ABC is applied simultaneously to multiple datasets. We test the results of the ABC inference by comparing the narrow-band magnitudes of the observed and simulated galaxies using Principal Component Analysis, finding a very good agreement. Furthermore, we prove the scientific potential of the constrained galaxy population model to provide realistic stellar population properties by measuring them with the SED fitting code \textsc{CIGALE}. We use CFHTLS broad-band and PAUS narrow-band photometry for a flux-limited ($\mathrm{i}, 53 pages, 17 figures, Accepted for publication in JCAP
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- 2021
8. Gravitation and the Universe from large scale-structures: The GAUSS mission concept Mapping the cosmic web up to the reionization era
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Stéphane Ilić, Emmanuel Gangler, Safir Yahia-Cherif, A. J. Hawken, Yann Rasera, Satya Gontcho A Gontcho, Jean-Paul Kneib, E. Aubourg, Norma G. Sanchez, Alain Blanchard, Guilhem Lavaux, Sandrine Codis, Julien Lesgourgues, Yannick Mellier, Olivier Le Fevre, C. Renault, Agnès Ferté, Fabien Dournac, Z. Sakr, Stephanie Escoffier, I. Tutusaus, M. Ricci, Philippe Brax, Pablo Fosalba, Fabio Finelli, Jérémy Neveu, Francisco J. Castander, Martin Kunz, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)
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Big Bang ,dark energy: parametrization ,satellite: Planck ,Primordial fluctuations ,media_common.quotation_subject ,Dark matter ,Observable universe ,Astrophysics::Cosmology and Extragalactic Astrophysics ,7. Clean energy ,01 natural sciences ,Cosmology ,dark matter: parametrization ,symbols.namesake ,cosmological model: parameter space ,0103 physical sciences ,ionization ,Dark energy ,structure ,[PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det] ,Planck ,010303 astronomy & astrophysics ,media_common ,Physics ,010308 nuclear & particles physics ,fluctuation: primordial ,Astrophysics::Instrumentation and Methods for Astrophysics ,big bang ,Astronomy ,Astronomy and Astrophysics ,space ,acceleration ,tensor ,Universe ,inflation: model ,13. Climate action ,Space and Planetary Science ,gravitation ,symbols ,galaxy: cluster ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Early Universe physics - Abstract
Blanchard, A., et al., Today, thanks in particular to the results of the ESA Planck mission, the concordance cosmological model appears to be the most robust to describe the evolution and content of the Universe from its early to late times. It summarizes the evolution of matter, made mainly of dark matter, from the primordial fluctuations generated by inflation around 10 second after the Big Bang to galaxies and clusters of galaxies, 13.8 billion years later, and the evolution of the expansion of space, with a relative slowdown in the matter-dominated era and, since a few billion years, an acceleration powered by dark energy. But we are far from knowing the pillars of this model which are inflation, dark matter and dark energy. Comprehending these fundamental questions requires a detailed mapping of our observable Universe over the whole of cosmic time. The relic radiation provides the starting point and galaxies draw the cosmic web. JAXA’s LiteBIRD mission will map the beginning of our Universe with a crucial test for inflation (its primordial gravity waves), and the ESA Euclid mission will map the most recent half part, crucial for dark energy. The mission concept GAUSS, described in this White Paper, aims at being a mission to fully map the cosmic web up to the reionization era, linking early and late evolution, to tackle and disentangle the crucial degeneracies persisting after the Euclid era between dark matter and inflation properties, dark energy, structure growth and gravitation at large scale.
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- 2021
9. Discovery of a Candidate Binary Supermassive Black Hole in a Periodic Quasar from Circumbinary Accretion Variability
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David J. James, Yu Ching Chen, Pablo Fosalba, David J. Brooks, Keith Bechtol, G. Gutierrez, Karl Glazebrook, Tim Eifler, V. Scarpine, Santiago Serrano, Flavia Sobreira, H. Thomas Diehl, Josh Frieman, Santiago Avila, Xin Liu, Carlos E. Cunha, Juan de Vicente, Shantanu Desai, Peter Doel, Jennifer L. Marshall, Juan Garcia-Bellido, Felipe Menanteau, Aurelio Carnero Rosell, Daniel Gruen, Emmanuel Bertin, Enrique Gaztanaga, Gregory Tarle, Richard Kessler, Mathew Smith, Ramon Miquel, B. Flaugher, J. Carretero, Matias Carrasco Kind, Devon L. Hollowood, Tamara M. Davis, K. Honscheid, Vinu Vikram, Marcos Lima, Richard G. McMahon, Hengxiao Guo, E. J. Sanchez, Molly E. C. Swanson, E. Suchyta, J. Gschwend, Elisabeth Krause, August E. Evrard, Yue Shen, Francisco J. Castander, Manda Banerji, Luiz N. da Costa, Paul Martini, Marcio A. G. Maia, R. Chris Smith, Christopher R. Davis, A. Miguel Holgado, Will Hartley, Eric Morganson, Ben Hoyle, S. Allam, Robert A. Gruendl, Andres Plazas Malagon, Kyler Kuehn, Chris B. D'Andrea, Alistair R. Walker, Marcelle Soares-Santos, Michael Schubnell, Wei-Ting Liao, E. Buckley-Geer, James Annis, A. Roodman, UAM. Departamento de Física Teórica, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Australian Research Council, and Instituto Nacional de Ciência e Tecnologia (Brasil)
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Astrophysics ,Surveys ,7. Clean energy ,01 natural sciences ,high-redshift [Galaxies] ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Data Release ,Galaxies: Active ,Dark Energy ,nuclei [Galaxies] ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Galaxy Mergers ,Digital Sky Survey ,Galaxies: Nuclei ,Oscillations ,active [Galaxies] ,QUASARES ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Gravitational-Waves ,0103 physical sciences ,Galaxy formation and evolution ,Quasars: General ,Astrophysics::Galaxy Astrophysics ,Supermassive black hole ,010308 nuclear & particles physics ,Gravitational wave ,Spectral Energy-Distributions ,Física ,Astronomy and Astrophysics ,Quasar ,general [Quasars] ,Black hole physics ,Mass ,Light curve ,Galaxies: High-Redshift ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Black Hole Physics ,13. Climate action ,Space and Planetary Science ,Variable Quasars ,Astrophysics of Galaxies (astro-ph.GA) ,Dark energy ,Galactic Nuclei ,Circumbinary planet ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
Binary supermassive black holes (BSBHs) are expected to be a generic byproduct from hierarchical galaxy formation. The final coalescence of BSBHs is thought to be the loudest gravitational wave (GW) siren, yet no confirmed BSBH is known in the GW-dominated regime. While periodic quasars have been proposed as BSBH candidates, the physical origin of the periodicity has been largely uncertain. Here, we report discovery of a periodicity (p = 1607 ± 7 d) at 99.95 per cent significance (with a global p value of ∼10-3 accounting for the look elsewhere effect) in the optical light curves of a redshift 1.53 quasar, SDSS J025214.67-002813.7. Combining archival Sloan Digital Sky Survey data with new, sensitive imaging from the Dark Energy Survey, the total ∼20-yr time baseline spans ∼4.6 cycles of the observed 4.4-yr (rest frame 1.7-yr) periodicity. The light curves are best fit by a bursty model predicted by hydrodynamic simulations of circumbinary accretion discs. The periodicity is likely caused by accretion rate modulation by a milli-parsec BSBH emitting GWs, dynamically coupled to the circumbinary accretion disc. A bursty hydrodynamic variability model is statistically preferred over a smooth, sinusoidal model expected from relativistic Doppler boost, a kinematic effect proposed for PG1302-102. Furthermore, the frequency dependence of the variability amplitudes disfavours Doppler boost, lending independent support to the circumbinary accretion variability hypothesis. Given our detection rate of one BSBH candidate from circumbinary accretion variability out of 625 quasars, it suggests that future large, sensitive synoptic surveys such as the Vera C. Rubin Observatory Legacy Survey of Space and Time may be able to detect hundreds to thousands of candidate BSBHs from circumbinary accretion with direct implications for Laser Interferometer Space Antenna., Liao, Wei-Ting, et al. DES Collaboration, The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and the Brazilian Instituto Nacional de Ciênciae Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).
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- 2020
10. CosmoHub : Interactive exploration and distribution of astronomical data on Hadoop
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Carles Acosta-Silva, Manuel Delfino, Nadia Tonello, Pablo Fosalba, Martin Crocce, Enrique Gaztanaga, Pau Tallada, S. Serrano, Francisco J. Castander, Martin Eriksen, G. Merino, J. Carretero, Marc Caubet, C. Neissner, Jordi Casals, Eduardo César, Ministerio de Ciencia, Innovación y Universidades (España), and European Commission
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Astronomical Objects ,FOS: Computer and information sciences ,SQL ,Data distribution ,Relational database ,Data exploration ,FOS: Physical sciences ,01 natural sciences ,ASDF ,0103 physical sciences ,Apache Hadoop ,Web application ,010303 astronomy & astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Digitization ,computer.programming_language ,Information retrieval ,010308 nuclear & particles physics ,business.industry ,End user ,Astronomy and Astrophysics ,Apache Hive ,Computer Science Applications ,Visualization ,Computer Science - Distributed, Parallel, and Cluster Computing ,Space and Planetary Science ,Physics - Data Analysis, Statistics and Probability ,Scalability ,FITS ,Distributed, Parallel, and Cluster Computing (cs.DC) ,Astrophysics - Instrumentation and Methods for Astrophysics ,business ,computer ,Data Analysis, Statistics and Probability (physics.data-an) - Abstract
We present CosmoHub (https://cosmohub.pic.es), a web application based on Hadoop to perform interactive exploration and distribution of massive cosmological datasets. Recent Cosmology seeks to unveil the nature of both dark matter and dark energy mapping the large-scale structure of the Universe, through the analysis of massive amounts of astronomical data, progressively increasing during the last (and future) decades with the digitization and automation of the experimental techniques. CosmoHub, hosted and developed at the Port d'Informació Científica (PIC), provides support to a worldwide community of scientists, without requiring the end user to know any Structured Query Language (SQL). It is serving data of several large international collaborations such as the Euclid space mission, the Dark Energy Survey (DES), the Physics of the Accelerating Universe Survey (PAUS) and the Marenostrum Institut de Ciències de l'Espai (MICE) numerical simulations. While originally developed as a PostgreSQL relational database web frontend, this work describes the current version of CosmoHub, built on top of Apache Hive, which facilitates scalable reading, writing and managing huge datasets. As CosmoHub's datasets are seldomly modified, Hive it is a better fit. Over 60 TiB of cataloged information and 50×10 astronomical objects can be interactively explored using an integrated visualization tool which includes 1D histogram and 2D heatmap plots. In our current implementation, online exploration of datasets of 10 objects can be done in a timescale of tens of seconds. Users can also download customized subsets of data in standard formats generated in few minutes., CosmoHub has been partially funded through projects of the Spanish national program “Programa Estatal de I + D + i” of the Spanish government. The support of the ERDF fund is gratefully acknowledged.
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- 2020
11. The PAU Survey: An improved photo-$z$ sample in the COSMOS field
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J. Carretero, Enrique Fernández, Juan de Vicente, Pablo Renard, Santiago Serrano, Laura Cabayol, C. Padilla, Juan Garcia-Bellido, Giorgio Manzoni, A. Alarcon, Enrique Gaztanaga, Benjamin Joachimi, Carlton M. Baugh, M. Siudek, Henk Hoekstra, P. Tallada-Crespí, E. J. Sanchez, Peder Norberg, Francisco J. Castander, Hendrik Hildebrandt, Martin Eriksen, Ramon Miquel, I. Sevilla-Noarbe, Ricard Casas, UAM. Departamento de Física Teórica, Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, European Commission, Durham University, Netherlands Organisation for Health Research and Development, Universidad Autónoma de Barcelona, and Ministerio de Ciencia, Innovación y Universidades (España)
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Accuracy and precision ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Photometry (optics) ,Evolution [Galaxies] ,Galaxies: Distances and Redshifts ,0103 physical sciences ,Galaxies: Evolution ,Galaxy formation and evolution ,Distances and Redshifts [Galaxies] ,Galaxies: Photometry ,Photometry [Galaxies] ,Linear combination ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,010308 nuclear & particles physics ,Spectral density ,Física ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Galaxy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Alarcon, A., et al., We present - and make publicly available - accurate and precise photometric redshifts in the ACS footprint from the COSMOS field for objects with iAB ≤ 23. The redshifts are computed using a combination of narrow-band photometry from PAUS, a survey with 40 narrow bands spaced at 100\,\mathring{\rm A} intervals covering the range from 4500 to 8500\,\mathring{\rm A}, and 26 broad, intermediate, and narrow bands covering the UV, visible and near-infrared spectrum from the COSMOS2015 catalogue. We introduce a new method that models the spectral energy distributions as a linear combination of continuum and emission-line templates and computes its Bayes evidence, integrating over the linear combinations. The correlation between the UV luminosity and the O ii line is measured using the 66 available bands with the zCOSMOS spectroscopic sample, and used as a prior which constrains the relative flux between continuum and emission-line templates. The flux ratios between the O ii line and Hα, Hβ and \mathrm{O\,{\small III}} are similarly measured and used to generate the emission-line templates. Comparing to public spectroscopic surveys via the quantity Δz (zphoto - zspec)/(1 + zspec), we find the photometric redshifts to be more precise than previous estimates, with σ68(Δz) ≈ (0.003, 0.009) for galaxies at magnitude iAB ∼18 and iAB ∼23, respectively, which is three times and 1.66 times tighter than COSMOS2015. Additionally, we find the redshifts to be very accurate on average, yielding a median of the Δz distribution compatible with |median(Δz)| ≤ 0.001 at all redshifts and magnitudes considered. Both the added PAUS data and new methodology contribute significantly to the improved results. The catalogue produced with the technique presented here is expected to provide a robust redshift calibration for current and future lensing surveys, and allows one to probe galaxy formation physics in an unexplored luminosity-redshift regime, thanks to its combination of depth, completeness, and excellent redshift precision and accuracy., Argonne National Laboratory’s work was supported by the US Department of Energy, Office of High Energy Physics. Argonne, a U.S. Department of Energy Office of Science Laboratory, is operated by UChicago Argonne LLC under contract no. DE-AC02-06CH11357. The PAU Survey is partially supported by MINECO under grantsCSD2007-00060, AYA2015-71825, ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, MDM-2015-0509 and Juan de la Cierva fellowship and LACEGAL and EWC Marie Sklodowska-Curie grant No 734374 and no. 776247 with ERDF funds from the EU Horizon 2020 Programme, some of which include ERDF funds from the European Union. IEEC and IFAE are partially funded by the CERCA and Beatriu de Pinos program of the Generalitat de Catalunya. Funding for PAUS has also been provided by Durham University (via the ERC StG DEGAS-259586), ETH Zurich, Leiden University (via ERC StG ADULT-279396 and Netherlands Organisation for Scientific Research (NWO) Vici grant 639.043.512), University College London and from the European Union’s Horizon 2020 research and innovation programme under the grant agreement No 776247 EWC. The PAU data centre is hosted by the Port d’Informació Científica (PIC), maintained through a collaboration of CIEMAT and IFAE, with additional support from Universitat Autònoma de Barcelona and ERDF. We acknowledge the PIC services department team for their support and fruitful discussions. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 776247. H. Hildebrandt is supported by a Heisenberg grant of the Deutsche Forschungsgemeinschaft (Hi 1495/5-1) as well as an ERC Consolidator Grant (No. 770935). H. Hoekstra acknowledges support from Vici grant 639.043.512 from the Netherlands Organization for Scientific Research (NWO). GM acknowledges support from ST/P006744/1. CMB acknowledges support from ST/P000541/1 and ST/T000244/1. PN acknowledges support from ST/P000541/1 and ST/T000244/1. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under the Maria Skłodowska-Curie (grant agreement No 754510), the National Science Centre of Poland (grant UMO-2016/23/N/ST9/02963) and by the Spanish Ministry of Science and Innovation through Juan de la Cierva-formacion program (reference FJC2018-038792-I).
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- 2020
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12. Trans-Neptunian Objects Found in the First Four Years of the Dark Energy Survey
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B. Flaugher, A. R. Walker, M. Carrasco Kind, Gary Bernstein, N. P. Kuropatkin, F. Paz-Chinchón, Carlos Solans Sanchez, Pedro H. Bernardinelli, Eli S. Rykoff, D. L. Burke, David James, Matthew Belyakov, William Wester, Larissa Markwardt, Hsing Wen Lin, Aditya Inada Somasundaram, P. Doel, A. K. Romer, Kyle Franson, Kevin Napier, J. De Vicente, M. Smith, Robert A. Gruendl, Juliette C. Becker, E. Suchyta, Tali Khain, M. E. C. Swanson, D. Gruen, Tongtian Liu, L. N. da Costa, T. M. C. Abbott, G. Gutierrez, V. Scarpine, Fred C. Adams, Ramon Miquel, William R. Saunders, D. W. Gerdes, H. T. Diehl, S. Desai, A. A. Plazas, Flavia Sobreira, Jennifer Locke, G. Tarle, I. Sevilla-Noarbe, Lakshay Sharma, M. W. G. Johnson, Santiago Avila, Elisabeth Krause, S. Everett, Francisco J. Castander, M. March, James Annis, Masao Sako, J. Gschwend, Devon L. Hollowood, E. J. Sanchez, D. Brooks, A. Carnero Rosell, M. A. G. Maia, Michael D. Johnson, D. J. Brout, Yanxi Zhang, Santiago Serrano, Juan Garcia-Bellido, National Science Foundation (US), National Aeronautics and Space Administration (US), Department of Energy (US), Ministerio de Ciencia e Innovación (España), Science and Technology Facilities Council (UK), University of Illinois, University of Chicago, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional das Fundaçôes Estaduais de Amparo à Pesquisa (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), German Research Foundation, University of Pennsylvania, Ministerio de Economía y Competitividad (España), European Commission, and Australian Research Council
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010504 meteorology & atmospheric sciences ,Trans-Neptunian objects ,media_common.quotation_subject ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,7. Clean energy ,Orbit determination ,0103 physical sciences ,Trans-Neptunian object ,010303 astronomy & astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,0105 earth and related environmental sciences ,media_common ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Astronomy and Astrophysics ,Transient detection ,Orbit ,13. Climate action ,Space and Planetary Science ,Sky ,Magnitude (astronomy) ,Dark energy ,Astronomy data analysis ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present a catalog of 316 trans-Neptunian bodies (TNOs) detected from the first four seasons ("Y4"data) of the Dark Energy Survey (DES). The survey covers a contiguous 5000 deg2 of the southern sky in the grizY optical/NIR filter set, with a typical TNO in this part of the sky being targeted by 25-30 Y4 exposures. This paper focuses on the methods used to detect these objects from the ≈60,000 Y4 exposures, a process made challenging by the absence of the few-hour repeat observations employed by TNO-optimized surveys. Newly developed techniques include: transient/moving object detection by comparison of single-epoch catalogs to catalogs of "stacked"images; quantified astrometric error from atmospheric turbulence; new software for detecting TNO linkages in a temporally sparse transient catalog, and for estimating the rate of spurious linkages; use of faint stars to determine the detection efficiency versus magnitude in all exposures. Final validation of the reality of linked orbits uses a new "sub-threshold confirmation"test, wherein we demand the object be detectable in a stack of the exposures in which the orbit indicates an object should be present, but was not individually detected. This catalog contains all validated TNOs which were detected on ≥6 unique nights in the Y4 data, and is complete to r ≲ 23.3 mag with virtually no dependence on orbital properties for bound TNOs at distance 30 au < d < 2500 au. The catalog includes 245 discoveries by DES, 139 not previously published. The final DES TNO catalog is expected to yield >0.3 mag more depth, and arcs of >4 yr for nearly all detections., University of Pennsylvania authors have been supported in this work by grants AST-1515804 and AST-1615555 from the National Science Foundation, and grant DE-SC0007901 from the Department of Energy. Work at University of Michigan is supported by the National Aeronautics and Space Administration under grant No. NNX17AF21G issued through the SSO Planetary Astronomy Program and NSF Graduate Research Fellowship grant No. DGE 1256260. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical-Infrared Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo InterAmerican Observatory, National Optical-Infrared Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007- 2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a nonexclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231. This research has made use of data and/or services provided by the International Astronomical Union’s Minor Planet Center (MPC). The authors thank Gareth Williams for assistance in the MPC object submission process.
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- 2020
13. Dark Energy Survey Year 1 Results: Constraining Baryonic Physics in the Universe
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Samuel Hinton, Elisabeth Krause, G. Gutierrez, Matthew R. Becker, Jochen Weller, David James, Matias Carrasco Kind, Marcelle Soares-Santos, E. Rozo, Timothy M. C. Abbott, Rachel Mandelbaum, James Annis, Aurelio Carnero Rosell, Ramon Miquel, Molly E. C. Swanson, D. L. Burke, Dragan Huterer, Hung Jin Huang, Robert A. Gruendl, Pablo Fosalba, E. J. Sanchez, Gary Bernstein, Andrés Plazas Malagón, Ofer Lahav, A. Roodman, Jennifer L. Marshall, C. Sánchez, Will Hartley, Judit Prat, Emmanuel Bertin, K. Romer, Francisco J. Castander, Mathew Smith, Michel Aguena, Santiago Serrano, B. Flaugher, Xiao Fang, I. Sevilla, Marcio A. G. Maia, V. Scarpine, Vivian Miranda, M. Gatti, Josh Frieman, Juan de Vicente, Jack Elvin-Poole, Peter Doel, Mike Jarvis, David J. Brooks, Enrique Gaztanaga, Tim Eifler, Anqi Chen, Luiz N. da Costa, F. Paz-Chinchón, Niall MacCrann, Diehl H. Thomas, Daniel Gruen, Simon Samuroff, J. DeRose, E. Suchyta, Ami Choi, Ben Hoyle, J. Carretero, J. P. Dietrich, Juan Garcia-Bellido, Oliver Friedrich, K. Honscheid, Felipe Menanteau, Gregory Tarle, S. Everett, Sukhdeep Singh, Markus Rau, Michael Troxel, Marcos Lima, Kyler Kuehn, Sarah Bridle, Santiago Avila, Joe Zuntz, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, UAM. Departamento de Física Teórica, and National Aeronautics and Space Administration (US)
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Particle physics ,Large-Scale Structure of Universe ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cosmic microwave background ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,7. Clean energy ,01 natural sciences ,Cosmology ,symbols.namesake ,cosmology: theory ,0103 physical sciences ,Planck ,cosmological parameters ,010303 astronomy & astrophysics ,Weak gravitational lensing ,Physics ,010308 nuclear & particles physics ,Física ,Astronomy and Astrophysics ,Galaxy ,Baryon ,13. Climate action ,Space and Planetary Science ,symbols ,Dark energy ,Theory [Cosmology] ,Cosmological Parameters ,Baryon acoustic oscillations ,large-scale structure of Universe ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Measurements of large-scale structure are interpreted using theoretical predictions for the matter distribution, including potential impacts of baryonic physics. We constrain the feedback strength of baryons jointly with cosmology using weak lensing and galaxy clustering observables (3$\times$2pt) of Dark Energy Survey (DES) Year 1 data in combination with external information from baryon acoustic oscillations (BAO) and Planck cosmic microwave background polarization. Our baryon modeling is informed by a set of hydrodynamical simulations that span a variety of baryon scenarios; we span this space via a Principal Component (PC) analysis of the summary statistics extracted from these simulations. We show that at the level of DES Y1 constraining power, one PC is sufficient to describe the variation of baryonic effects in the observables, and the first PC amplitude ($Q_1$) generally reflects the strength of baryon feedback. With the upper limit of $Q_1$ prior being bound by the Illustris feedback scenarios, we reach $\sim 20\%$ improvement in the constraint of $S_8=\sigma_8(\Omega_{\rm m}/0.3)^{0.5}=0.788^{+0.018}_{-0.021}$ compared to the original DES 3$\times$2pt analysis. This gain is driven by the inclusion of small-scale cosmic shear information down to 2.5 arcmin, which was excluded in previous DES analyses that did not model baryonic physics. We obtain $S_8=0.781^{+0.014}_{-0.015}$ for the combined DES Y1+Planck EE+BAO analysis with a non-informative $Q_1$ prior. In terms of the baryon constraints, we measure $Q_1=1.14^{+2.20}_{-2.80}$ for DES Y1 only and $Q_1=1.42^{+1.63}_{-1.48}$ for DESY1+Planck EE+BAO, allowing us to exclude one of the most extreme AGN feedback hydrodynamical scenario at more than $2 \sigma$., Comment: 22 pages, 18 figures, 2 tables. accepted to MNRAS. A brief video summary of this paper is available at https://www.youtube.com/watch?v=QbeNwk5papU
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- 2020
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14. Dark Energy Survey Year 1 Results:Constraints on Intrinsic Alignments and their Colour Dependence from Galaxy Clustering and Weak Lensing
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Juan Garcia-Bellido, J. Carretero, Elisabeth Krause, I. Sevilla-Noarbe, Erin Sheldon, David Brooks, J. P. Dietrich, Daniel Gruen, N. Kuropatkin, D. W. Gerdes, J. De Vicente, R. H. Schindler, R. L. C. Ogando, L. N. da Costa, E. Suchyta, Ramon Miquel, Marcos Lima, S. Serrano, Peter Doel, Peter Melchior, Francisco J. Castander, D. L. DePoy, Michael Troxel, M. A. G. Maia, Vinu Vikram, A. Carnero Rosell, M. March, A. A. Plazas, T. M. C. Abbott, Kyler Kuehn, Joshua A. Frieman, M. Carrasco Kind, Michael Schubnell, P. Larsen, Christopher J. Miller, Daniel Thomas, S. Samuroff, V. Scarpine, Tim Eifler, Flavia Sobreira, E. J. Sanchez, Jonathan Blazek, David J. James, W. G. Hartley, M. Gatti, Niall MacCrann, Enrique Gaztanaga, Devon L. Hollowood, C. D. Leonard, J. Prat, Sarah Bridle, Scott Dodelson, Pablo Fosalba, B. Flaugher, Carlos E. Cunha, Ben Hoyle, G. Gutierrez, Joe Zuntz, Shantanu Desai, H. T. Diehl, Mathew Smith, E. Bertin, C. Davis, J. Gschwend, Gary Bernstein, S. Allam, Robert A. Gruendl, Paul Martini, Felipe Menanteau, Gregory Tarle, K. Honscheid, J. Annis, Jennifer L. Marshall, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
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luminous red galaxies ,Astrophysics and Astronomy ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cosmological parameters ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Cosmology ,contamination ,gravitational lensing: weak ,statistics [Galaxies] ,TheoryofComputation_ANALYSISOFALGORITHMSANDPROBLEMCOMPLEXITY ,0103 physical sciences ,cosmological parameters ,observations [Cosmology] ,010303 astronomy & astrophysics ,Weak gravitational lensing ,galaxies: statistics ,Astrophysics::Galaxy Astrophysics ,Photometric redshift ,Physics ,cosmological parameter constraints ,model ,Series (mathematics) ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Redshift ,Galaxy ,Amplitude ,kids-450 ,Space and Planetary Science ,cosmology: observations ,Dark energy ,impact ,astro-ph.CO ,High Energy Physics::Experiment ,digital sky survey ,Astrophysics::Earth and Planetary Astrophysics ,weak [Gravitational lensing] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,cosmic shear ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We perform a joint analysis of intrinsic alignments and cosmology using tomographic weak lensing, galaxy clustering and galaxy-galaxy lensing measurements from Year 1 (Y1) of the Dark Energy Survey. We define early- and late-type subsamples, which are found to pass a series of systematics tests, including for spurious photometric redshift error and point spread function correlations. We analyse these split data alongside the fiducial mixed Y1 sample using a range of intrinsic alignment models. In a fiducial Nonlinear Alignment Model (NLA) analysis, assuming a flat \lcdm~cosmology, we find a significant difference in intrinsic alignment amplitude, with early-type galaxies favouring $A_\mathrm{IA} = 2.38^{+0.32}_{-0.31}$ and late-type galaxies consistent with no intrinsic alignments at $0.05^{+0.10}_{-0.09}$. We find weak evidence of a diminishing alignment amplitude at higher redshifts in the early-type sample. The analysis is repeated using a number of extended model spaces, including a physically motivated model that includes both tidal torquing and tidal alignment mechanisms. In multiprobe likelihood chains in which cosmology, intrinsic alignments in both galaxy samples and all other relevant systematics are varied simultaneously, we find the tidal alignment and tidal torquing parts of the intrinsic alignment signal have amplitudes $A_1 = 2.66 ^{+0.67}_{-0.66}$, $A_2=-2.94^{+1.94}_{-1.83}$, respectively, for early-type galaxies and $A_1 = 0.62 ^{+0.41}_{-0.41}$, $A_2 = -2.26^{+1.30}_{-1.16}$ for late-type galaxies. In the full (mixed) Y1 sample the best constraints are $A_1 = 0.70 ^{+0.41}_{-0.38}$, $A_2 = -1.36 ^{+1.08}_{-1.41}$. For all galaxy splits and IA models considered, we report cosmological parameter constraints that are consistent with the results of Troxel et al. (2017) and Dark Energy Survey Collaboration (2017)., 31 pages, 23 figures; accepted by MNRAS
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- 2019
15. H0LiCOW - X. Spectroscopic/imaging survey and galaxy-group identification around the strong gravitational lens system WFI 2033-4723
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Sherry H. Suyu, Stefan Hilbert, D. L. Burke, Peter Doel, Robert A. Gruendl, Kenneth C. Wong, Cristian E. Rusu, M. Carrasco Kind, Juan Garcia-Bellido, A. A. Plazas, M. A. G. Maia, Simon Birrer, David J. Brooks, Elisabeth Krause, Matthew W. Auger, W. G. Hartley, Philip J. Marshall, Luitje Koopmans, H. Lin, Anowar J. Shajib, Vivien Bonvin, E. Buckley-Geer, M. Lima, David Goldstein, J. Carretero, Johan Richard, S. Serrano, J. De Vicente, Dominique Sluse, E. Suchyta, Ramon Miquel, August E. Evrard, Thomas E. Collett, Marcelle Soares-Santos, E. Bertin, J. Gschwend, Frederic Courbin, Christopher D. Fassnacht, Flavia Sobreira, E. J. Sanchez, Alessandro Sonnenfeld, G. Meylan, Shantanu Desai, Felipe Menanteau, Santiago Avila, Lodovico Coccato, D. L. Hollowood, A. G. Kim, Francisco J. Castander, M. Smith, D. W. Gerdes, David J. James, B. Flaugher, K. Honscheid, O. Tihhanova, Jennifer L. Marshall, Peter Melchior, Joshua A. Frieman, J. Annis, G. Tarle, Adriano Agnello, I. Sevilla-Noarbe, N. Kuropatkin, L. N. da Costa, A. Carnero Rosell, Kyler Kuehn, Tommaso Treu, M. E. C. Swanson, Astronomy, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
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High energy ,Higher education ,astro-ph.GA ,REDSHIFT ,FOS: Physical sciences ,Library science ,COSMOGRAIL ,Astrophysics::Cosmology and Extragalactic Astrophysics ,MULTIWAVELENGTH SURVEY ,Astronomy & Astrophysics ,MASS ,01 natural sciences ,galaxies: groups: general ,0103 physical sciences ,media_common.cataloged_instance ,Astrophysics::Solar and Stellar Astrophysics ,European union ,DEEP FIELD-SOUTH ,010303 astronomy & astrophysics ,YALE-CHILE MUSYC ,STFC ,Astrophysics::Galaxy Astrophysics ,media_common ,Physics ,International research ,HAWK-I ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,business.industry ,groups: general [galaxies] ,European research ,individual: WFI 2033-4723 [quasars] ,RCUK ,gravitational lensing: strong ,Astronomy and Astrophysics ,Chinese academy of sciences ,Astrophysics - Astrophysics of Galaxies ,CATALOG ,STELLAR ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Astrophysics of Galaxies (astro-ph.GA) ,strong [gravitational lensing] ,quasars: individual: WFI 2033-4723 ,Christian ministry ,Space Science ,business ,Astronomical and Space Sciences ,HUBBLE CONSTANT - Abstract
Galaxies and galaxy groups located along the line of sight towards gravitationally lensed quasars produce high-order perturbations of the gravitational potential at the lens position. When these perturbation are too large, they can induce a systematic error on $H_0$ of a few-percent if the lens system is used for cosmological inference and the perturbers are not explicitly accounted for in the lens model. In this work, we present a detailed characterization of the environment of the lens system WFI2033-4723 ($z_{\rm src} = 1.662$, $z_{\rm lens}$ = 0.6575), one of the core targets of the H0LICOW project for which we present cosmological inferences in a companion paper (Rusu et al. 2019). We use the Gemini and ESO-Very Large telescopes to measure the spectroscopic redshifts of the brightest galaxies towards the lens, and use the ESO-MUSE integral field spectrograph to measure the velocity-dispersion of the lens ($\sigma_{\rm {los}}= 250^{+15}_{-21}$ km/s) and of several nearby galaxies. In addition, we measure photometric redshifts and stellar masses of all galaxies down to $i < 23$ mag, mainly based on Dark Energy Survey imaging (DR1). Our new catalog, complemented with literature data, more than doubles the number of known galaxy spectroscopic redshifts in the direct vicinity of the lens, expanding to 116 (64) the number of spectroscopic redshifts for galaxies separated by less than 3 arcmin (2 arcmin) from the lens. Using the flexion-shift as a measure of the amplitude of the gravitational perturbation, we identify 2 galaxy groups and 3 galaxies that require specific attention in the lens models. The ESO MUSE data enable us to measure the velocity-dispersions of three of these galaxies. These results are essential for the cosmological inference analysis presented in Rusu et al. (2019)., Comment: Matches the version accepted for publication by MNRAS. Note that this paper previously appeared as H0LICOW XI
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- 2019
16. Galaxies in X-ray selected clusters and groups in dark energy survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function
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A. A. Plazas, J. Gschwend, B. Flaugher, E. Suchyta, Martin Sahlén, Chris A. Collins, Matt Hilton, Flavia Sobreira, Daniel Gruen, M. A. G. Maia, Felipe Menanteau, Martin Crocce, Gregory Tarle, Michael Schubnell, Robert G. Mann, D. W. Gerdes, John P. Stott, J. Carretero, G. Gutierrez, K. Honscheid, M. March, Mathew Smith, H. T. Diehl, J. P. Dietrich, David Bacon, Risa H. Wechsler, N. Kuropatkin, C. B. D'Andrea, Eli S. Rykoff, C. J. Miller, P. Rooney, Rituparna Das, A. Benoit-Lévy, David J. James, David J. Brooks, Enrique Gaztanaga, Ramon Miquel, Pablo Fosalba, A. Bermeo, Juan Garcia-Bellido, Julian A. Mayers, A. Carnero Rosell, Francisco J. Castander, Filipe B. Abdalla, M. Carrasco Kind, Robert C. Nichol, J. Song, E. Buckley-Geer, C. Vergara Cervantes, Marcos Lima, Alistair R. Walker, Marcelle Soares-Santos, I. Sevilla-Noarbe, L. N. da Costa, R. L. C. Ogando, C. Hennig, M. E. C. Swanson, Timothy A. McKay, Yanxi Zhang, Tim Eifler, H. Wilcox, Jennifer L. Marshall, Ben Hoyle, Nicola Mehrtens, Peter Melchior, Kyler Kuehn, A. K. Romer, Andrew R. Liddle, Sarah Bridle, Carlos E. Cunha, Pedro T. P. Viana, T. M. C. Abbott, E. J. Sanchez, Scott T. Kay, Han Lin, D. L. Burke, S. Allam, Robert A. Gruendl, Tesla E. Jeltema, C. J. Conselice, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Evolution ,Astrophysics::High Energy Astrophysical Phenomena ,astro-ph.GA ,General – galaxies ,Bayesian probability ,AST-1138766 ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Clusters ,Astronomi, astrofysik och kosmologi ,0103 physical sciences ,Cluster (physics) ,Astrophysics::Solar and Stellar Astrophysics ,Astronomy, Astrophysics and Cosmology ,clusters: general [galaxies] ,AST-1536171 ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,QC ,evolution [galaxies] ,STFC ,Luminosity function (astronomy) ,QB ,Physics ,Sequence ,010308 nuclear & particles physics ,RCUK ,Astronomy and Astrophysics ,Function (mathematics) ,Galaxies ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Space and Planetary Science ,galaxies: clusters: general ,Astrophysics of Galaxies (astro-ph.GA) ,Dark energy ,astro-ph.CO ,Survey data collection ,galaxies: evolution ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Using $\sim 100$ X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function (LF) of cluster red sequence galaxies as a function of redshift. This is the first homogeneous optical/X-ray sample large enough to constrain the evolution of the luminosity function simultaneously in redshift ($0.1, Comment: Updated to match the accepted version
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- 2019
17. The Complete Calibration of the Color–Redshift Relation (C3R2) Survey : analysis and data release 2
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Francisco J. Castander, Iary Davidzon, Peter Capak, S. Adam Stanford, Nina Hernitschek, D. B. Sanders, Audrey Galametz, Jason Rhodes, Kerianne Pruett, Bahram Mobasher, Sotiria Fotopoulou, Daniel Stern, Daniel Masters, and Judith G. Cohen
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Physics ,Brightness ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010504 meteorology & atmospheric sciences ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Color space ,Astrophysics - Astrophysics of Galaxies ,01 natural sciences ,Galaxy ,Cosmology ,Redshift ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Calibration ,Dark energy ,010303 astronomy & astrophysics ,Weak gravitational lensing ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics ,0105 earth and related environmental sciences - Abstract
The Complete Calibration of the Color-Redshift Relation (C3R2) survey is a multi-institution, multi-instrument survey that aims to map the empirical relation of galaxy color to redshift to i~24.5 (AB), thereby providing a firm foundation for weak lensing cosmology with the Stage IV dark energy missions Euclid and WFIRST. Here we present 3171 new spectroscopic redshifts obtained in the 2016B and 2017A semesters with a combination of DEIMOS, LRIS, and MOSFIRE on the Keck telescopes. The observations come from all of the Keck partners: Caltech, NASA, the University of Hawaii, and the University of California. Combined with the 1283 redshifts published in DR1, the C3R2 survey has now obtained and published 4454 high quality galaxy redshifts. We discuss updates to the survey design and provide a catalog of photometric and spectroscopic data. Initial tests of the calibration method performance are given, indicating that the sample, once completed and combined with extensive data collected by other spectroscopic surveys, should allow us to meet the cosmology requirements for Euclid, and make significant headway toward solving the problem for WFIRST. We use the full spectroscopic sample to demonstrate that galaxy brightness is weakly correlated with redshift once a galaxy is localized in the Euclid or WFIRST color space, with potentially important implications for the spectroscopy needed to calibrate redshifts for faint WFIRST and LSST sources., Comment: ApJ accepted. Survey website with links to the C3R2 redshift catalog and spectroscopic data hosted by KOA can be found at https://sites.google.com/view/c3r2-survey/home
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- 2019
18. First Cosmology Results Using Type Ia Supernovae from the Dark Energy Survey: Photometric Pipeline and Light-curve Data Release
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Anais Möller, J. Carretero, Tamara M. Davis, Daniel A. Goldstein, M. S. Schubnell, Richard Kessler, Douglas L. Tucker, Peter Nugent, Martin Crocce, H. T. Diehl, C. B. D'Andrea, Alex G. Kim, W. G. Hartley, S. Serrano, Ken Herner, David J. James, Flavia Sobreira, Bruce A. Bassett, Lluís Galbany, N. P. Kuropatkin, Devon L. Hollowood, T. M. C. Abbott, Daniel Gruen, Enrique Gaztanaga, Pablo Fosalba, E. Suchyta, J. Frieman, E. J. Sanchez, Yanxi Zhang, Tim Eifler, Paul Martini, A. Roodman, M. March, D. W. Gerdes, Brian Yanny, Yen-Chen Pan, C. Davis, A. A. Plazas, L. N. da Costa, Shantanu Desai, Mark Sullivan, M. Carrasco Kind, Robert C. Nichol, Peter de Nully Brown, E. Kasai, Mathew Smith, S. Allam, Robert A. Gruendl, David Brooks, M. E. C. Swanson, Francisco J. Castander, Daniel Scolnic, A. Carnero Rosell, J. De Vicente, Carlos Cunha, Ofer Lahav, Marco A. P. Lima, Brian Nord, Juan Garcia-Bellido, J. Lasker, Samuel Hinton, Tenglin Li, Santiago Avila, R. C. Thomas, J. Gschwend, G. Gutierrez, D. J. Brout, Eric Morganson, Masao Sako, William Wester, Ryan J. Foley, Edward Macaulay, Kyler Kuehn, V. Scarpine, Daniel Thomas, Emmanuel Bertin, Alistair R. Walker, Marcelle Soares-Santos, Rafe Schindler, Jennifer L. Marshall, Brad E. Tucker, Gregory Tarle, K. Honscheid, Eli S. Rykoff, D. L. Burke, I. Sevilla-Noarbe, R. Wolf, B. Flaugher, James Annis, M. Childress, Ramon Miquel, P. Doel, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
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010504 meteorology & atmospheric sciences ,Pipeline (computing) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Cosmology ,techniques: photometric ,supernovae: general ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Surface brightness ,[PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det] ,010303 astronomy & astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,STFC ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,RCUK ,Astronomy and Astrophysics ,Function (mathematics) ,Light curve ,Galaxy ,Supernova ,Space and Planetary Science ,cosmology: observations ,Dark energy ,SUPERNOVAS ,Astrophysics - Instrumentation and Methods for Astrophysics ,astro-ph.IM - Abstract
We present griz light curves of 251 Type Ia Supernovae (SNe Ia) from the first 3 years of the Dark Energy Survey Supernova Program's (DES-SN) spectroscopically classified sample. The photometric pipeline described in this paper produces the calibrated fluxes and associated uncertainties used in the cosmological parameter analysis (Brout et al. 2018-SYS, DES Collaboration et al. 2018) by employing a scene modeling approach that simultaneously forward models a variable transient flux and temporally constant host galaxy. We inject artificial point sources onto DECam images to test the accuracy of our photometric method. Upon comparison of input and measured artificial supernova fluxes, we find flux biases peak at 3 mmag. We require corrections to our photometric uncertainties as a function of host galaxy surface brightness at the transient location, similar to that seen by the DES Difference Imaging Pipeline used to discover transients. The public release of the light curves can be found at https://des.ncsa.illinois.edu/releases/sn., Comment: 12 Pages, 8 Figures, Submitted to ApJ, Comments welcome
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- 2019
19. The Physics of the Accelerating Universe Camera
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José M. Illa, Enrique Fernández, J. Carretero, Pau Tallada, M. Delfino, Carlos Díaz, I. Sevilla-Noarbe, Martin Crocce, Juan de Vicente, Francisco J. Castander, Javier Castilla, Juan Garcia-Bellido, A. Alarcon, Martin Eriksen, Luis Lopez, C. Neissner, Jelena Aleksić, S. Serrano, Cristóbal Pío, Pablo Fosalba, Laia Cardiel-Sas, Ramon Miquel, Nadia Tonello, Laura Cabayol, Cristobal Padilla, Ricard Casas, O. Ballester, Ferran Grañena, Pol Martí, Enrique Gaztanaga, J. Gaweda, E. J. Sanchez, and Jorge Jiménez
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Physics ,010504 meteorology & atmospheric sciences ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,FOS: Physical sciences ,Astronomy and Astrophysics ,Field of view ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Galaxy ,Redshift ,Photometry (optics) ,Cardinal point ,Space and Planetary Science ,0103 physical sciences ,William Herschel Telescope ,Galaxy formation and evolution ,Spectral energy distribution ,Astrophysics - Instrumentation and Methods for Astrophysics ,010303 astronomy & astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences - Abstract
The PAU (Physics of the Accelerating Universe) Survey goal is to obtain photometric redshifts (photo-z) and Spectral Energy Distribution (SED) of astronomical objects with a resolution roughly one order of magnitude better than current broad band photometric surveys. To accomplish this, a new large field of view camera (PAUCam) has been designed, built, commissioned and is now operated at the William Herschel Telescope (WHT). With the current WHT Prime Focus corrector, the camera covers ~1-degree diameter Field of View (FoV), of which, only the inner ~40 arcmin diameter are unvignetted. The focal plane consists of a mosaic of 18 2k$x4k Hamamatsu fully depleted CCDs, with high quantum efficiency up to 1 micrometers in wavelength. To maximize the detector coverage within the FoV, filters are placed in front of the CCDs inside the camera cryostat (made out of carbon fiber) using a challenging movable tray system. The camera uses a set of 40 narrow band filters ranging from ~4500 to ~8500 Angstroms complemented with six standard broad-band filters, ugrizY. The PAU Survey aims to cover roughly 100 square degrees over fields with existing deep photometry and galaxy shapes to obtain accurate photometric redshifts for galaxies down to i_AB~22.5, detecting also galaxies down to i_AB~24 with less precision in redshift. With this data set we will be able to measure intrinsic alignments, galaxy clustering and perform galaxy evolution studies in a new range of densities and redshifts. Here, we describe the PAU camera, its first commissioning results and performance., 34 pages, 55 figures
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- 2019
20. Mass variance from archival X-ray properties of Dark Energy Survey Year-1 galaxy clusters
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Peter Doel, Elisabeth Krause, David J. James, Alistair R. Walker, Pablo Fosalba, H. T. Diehl, Douglas L. Tucker, J. Carretero, Jochen Weller, Pedro T. P. Viana, Kyler Kuehn, E. J. Sanchez, Paul Giles, I. Sevilla-Noarbe, Eli S. Rykoff, David Brooks, M. E. C. Swanson, N. Kuropatkin, Shantanu Desai, J. P. Dietrich, Ramon Miquel, Adam Mantz, L. N. da Costa, Mathew Smith, M. Carrasco Kind, A. Bermeo, C. Vergara Cervantes, Daniel Thomas, Marcos Lima, E. Buckley-Geer, Xi Chen, V. Scarpine, R. L. C. Ogando, Tesla E. Jeltema, Sunayana Bhargava, Michael Schubnell, Joshua A. Frieman, G. Gutierrez, Robert G. Mann, Jennifer L. Marshall, J. Gschwend, K. Honscheid, Enrique Gaztanaga, M. Costanzi, Yanxi Zhang, Julian A. Mayers, A. K. Romer, August E. Evrard, Arya Farahi, Flavia Sobreira, S. Serrano, Felipe Menanteau, B. Flaugher, John P. Stott, Gregory Tarle, R. D. Wilkinson, A. Carnero Rosell, S. Everett, P. Rooney, D. L. Burke, Juan Garcia-Bellido, Martin Sahlén, Chris A. Collins, Eduardo Rozo, J. Annis, Robert A. Gruendl, Vinu Vikram, J. De Vicente, E. Suchyta, Matt Hilton, Santiago Avila, Devon L. Hollowood, Andrew R. Liddle, Francisco J. Castander, A. A. Plazas, Daniel Gruen, D. W. Gerdes, M. A. G. Maia, Peter Melchior, Farahi, A., Chen, X., Evrard, A. E., Hollowood, D. L., Wilkinson, R., Bhargava, S., Giles, P., Romer, A. K., Jeltema, T., Hilton, M., Bermeo, A., Mayers, J., Vergara Cervantes, C., Rozo, E., Rykoff, E. S., Collins, C., Costanzi, M., Everett, S., Liddle, A. R., Mann, R. G., Mantz, A., Rooney, P., Sahlen, M., Stott, J., Viana, P. T. P., Zhang, Y., Annis, J., Avila, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., da Costa, L. N., de Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Plazas, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., and Weller, J.
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,astro-ph.GA ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,clusters: general [Galaxies] ,01 natural sciences ,0103 physical sciences ,010306 general physics ,GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries) ,010303 astronomy & astrophysics ,Scaling ,STFC ,ComputingMilieux_MISCELLANEOUS ,QC ,Galaxy cluster ,QB ,Confidence region ,Physics ,clusters: general - X-rays: galaxies: clusters [Galaxies] ,RCUK ,Astronomy and Astrophysics ,Covariance ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Redshift ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Log-normal distribution ,astro-ph.CO ,Galaxies: clusters: general - X-rays: galaxies: clusters ,galaxies: clusters [X-rays] ,Halo ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Using archival X-ray observations and a log-normal population model, we estimate constraints on the intrinsic scatter in halo mass at fixed optical richness for a galaxy cluster sample identified in Dark Energy Survey Year-One (DES-Y1) data with the redMaPPer algorithm. We examine the scaling behavior of X-ray temperatures, $T_X$, with optical richness, $\lambda_{RM}$, for clusters in the redshift range $0.2 50\%$ complete for clusters with $\lambda_{RM} > 130$. Regression analysis on the two samples produces consistent posterior scaling parameters, from which we derive a combined constraint on the residual scatter, $\sigma_{\ln Tx | \lambda} = 0.275 \pm 0.019$. Joined with constraints for $T_X$ scaling with halo mass from the Weighing the Giants program and richness--temperature covariance estimates from the LoCuSS sample, we derive the richness-conditioned scatter in mass, $\sigma_{\ln M | \lambda} = 0.30 \pm 0.04\, _{({\rm stat})} \pm 0.09\, _{({\rm sys})}$, at an optical richness of approximately 70. Uncertainties in external parameters, particularly the slope and variance of the $T_X$--mass relation and the covariance of $T_X$ and $\lambda_{RM}$ at fixed mass, dominate the systematic error. The $95\%$ confidence region from joint sample analysis is relatively broad, $\sigma_{\ln M | \lambda} \in [0.14, \, 0.55]$, or a factor ten in variance., Comment: 14 pages. Main results are Figure 3, 5, and 6, Table 2, and Equation 9. Submitted to MNRAS. Comments welcome
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- 2019
21. The ALHAMBRA survey: tight dependence of the optical mass-to-light ratio on galaxy colour up to z = 1.5
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A. del Olmo, Alberto Fernández-Soto, C. Husillos, J. Perea, I. Márquez, C. López-Sanjuan, Pablo Arnalte-Mur, Alberto Molino, Mirjana Pović, David Cristóbal-Hornillos, Francisco J. Castander, Kerttu Viironen, Jesús A. Varela, A. J. Cenarro, Mariano Moles, Miguel Cerviño, L. A. Díaz-García, R. M. González Delgado, Narciso Benítez, B. Ascaso, J. Masegosa, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Ministry of Science and Technology (Ethiopia), Governo Brasil, Generalitat de Catalunya, Junta de Andalucía, Generalitat Valenciana, European Commission, Fundación Agencia Aragonesa para la Investigación y el Desarrollo, Ministerio de Ciencia e Innovación (España), Fondo de Inversiones de Teruel, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
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Research groups ,Library science ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,statistics [Galaxies] ,0103 physical sciences ,media_common.cataloged_instance ,Astrophysics::Solar and Stellar Astrophysics ,European union ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,galaxies: statistics ,media_common ,Funding Agency ,Physics ,[PHYS]Physics [physics] ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,galaxies: fundamental parameters ,Astrophysics - Astrophysics of Galaxies ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,fundamental parameters [Galaxies] ,galaxies: stellar content ,stellar content [Galaxies] ,Christian ministry - Abstract
[Aims] Our goal is to characterise the dependence of the optical mass-to-light ratio on galaxy colour up to z = 1.5, expanding the redshift range explored in previous work. [Methods] From the redshifts, stellar masses, and rest-frame luminosities of the ALHAMBRA multi-filter survey, we derive the mass-to-light ratio versus colour relation for quiescent and for star-forming galaxies. The intrinsic relation and its physical dispersion are derived with a Bayesian inference model. [Results] The rest-frame i-band mass-to-light ratio of quiescent and star-forming galaxies presents a tight correlation with the rest-frame (g - i) colour up to z = 1.5. The mass-to-light ratio versus colour relation is linear for quiescent galaxies and quadratic for star-forming galaxies. The intrinsic dispersion in these relations is 0.02 dex for quiescent galaxies and 0.06 dex for star-forming ones. The derived relations do not present a significant redshift evolution and are compatible with previous local results in the literature. Finally, these tight relations also hold for g- and r-band luminosities. [Conclusions] The derived mass-to-light ratio versus colour relations in ALHAMBRA can be used to predict the mass-to-light ratio from a rest-frame optical colour up to z = 1.5. These tight correlations do not change with redshift, suggesting that galaxies have evolved along the derived relations during the last 9 Gyr., This work has been mainly funded by the FITE (Fondos de Inversiones de Teruel) and the Spanish MINECO/FEDER projects AYA2015-66211-C2-1-P, AYA2012-30789, AYA2006-14056, and CSD2007-00060. We also acknowledge the financial support from the Aragón Government Research Groups E96, E103, and E16_17R. We acknowledge support from the Spanish Ministry for Economy and Competitiveness and FEDER funds through grants AYA2010-15081, AYA2010-22111-C03-01, AYA2010-22111-C03-02, AYA2012-39620, AYA2013-40609-P, AYA2013-42227-P, AYA2013-48623-C2-1, AYA2013-48623-C2-2, AYA2016-76682-C3-1-P, AYA2016-76682-C3-3-P, ESP2013-48274, Generalitat Valen-ciana project Prometeo PROMETEOII/2014/060, Junta de Andalucía grants TIC114, JA2828, P10-FQM-6444, and Generalitat de Catalunya project SGR-1398. K.V. acknowledges the Juan de la Cierva incorporación fellowship, IJCI-2014-21960, of the Spanish government. A.M. acknowledges the financial support of the Brazilian funding agency FAPESP (Post-doc fellowship - process number 2014/11806-9). B.A. has received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No. 656354. M.P. acknowledges financial support from the Ethiopian Space Science and Technology Institute (ESSTI) under the Ethiopian Ministry of Science Science and Technology (MoST).
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- 2019
22. A new method to measure galaxy bias by combining the density and weak lensing fields
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Martin Crocce, Enrique Gaztanaga, Chihway Chang, Marc Manera, J. Carretero, Pablo Fosalba, Alexandre Refregier, Adam Amara, Francisco J. Castander, David Bacon, Vinu Vikram, and Arnau Pujol
- Subjects
Cosmology and Gravitation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Field (physics) ,Strong gravitational lensing ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,Measure (mathematics) ,Cosmology ,weak [gravitational lensing] ,0103 physical sciences ,Convergence (routing) ,survey ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Weak gravitational lensing ,Physics ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Galaxy ,Gravitational lens ,Space and Planetary Science ,astro-ph.CO ,large-scale structure of Universe ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present a new method to measure the redshift-dependent galaxy bias by combining information from the galaxy density field and the weak lensing field. This method is based on Amara et al. (2012), where they use the galaxy density field to construct a bias-weighted convergence field kg. The main difference between Amara et al. (2012) and our new implementation is that here we present another way to measure galaxy bias using tomography instead of bias parameterizations. The correlation between kg and the true lensing field k allows us to measure galaxy bias using different zero-lag correlations, such as / or /. Our method measures the linear bias factor on linear scales under the assumption of no stochasticity between galaxies and matter. We use the MICE simulation to measure the linear galaxy bias for a flux-limited sample (i < 22.5) in tomographic redshift bins using this method. This paper is the first that studies the accuracy and systematic uncertainties associated with the implementation of the method, and the regime where it is consistent with the linear galaxy bias defined by projected 2-point correlation functions (2PCF). We find that our method is consistent with linear bias at the percent level for scales larger than 30 arcmin, while nonlinearities appear at smaller scales. This measurement is a good complement to other measurements of bias, since it does not depend strongly on sigma8 as the 2PCF measurements. We apply this method to the Dark Energy Survey Science Verification data in a follow-up paper., Comment: 15 pages, 9 figures
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- 2016
23. High redshift galaxies in the ALHAMBRA survey. II. Strengthening the evidence of bright-end excess in UV luminosity functions at 2.5 <= z<= 4.5 by PDF analysis
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A. J. Cenarro, Mirjana Pović, Francisco Prada, A. del Olmo, Mariano Moles, Alberto Fernández-Soto, Alberto Molino, J. Varela, J. M. Quintana, C. Hernández-Monteagudo, Miguel Cerviño, Vivian Martínez, Narciso Benítez, Emilio J. Alfaro, I. Márquez, J. Masegosa, C. Husillos, Tom Broadhurst, Kerttu Viironen, L. A. Díaz-García, T. Aparicio-Villegas, Jonás Chaves-Montero, Jesús Cabrera-Caño, R. M. González Delgado, Jaime Perea, C. López-Sanjuan, J. A. L. Aguerri, B. Ascaso, Leopoldo Infante, S. Bonoli, Francisco J. Castander, David Cristóbal-Hornillos, J. Cepa, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Spanish National Research Council (CSIC), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Services communs OMP (UMS 831), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), AUTRES, Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 'Federico II' University of Naples Medical School, INTA - Instituto Nacional de Tecnología Agropecuaria, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Services communs OMP - UMS 831 (UMS 831), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Generalitat Valenciana, Junta de Andalucía, Generalitat de Catalunya, Fundación Agencia Aragonesa para la Investigación y el Desarrollo, Fondo de Inversiones de Teruel, European Commission, Ministry of Science and Technology (Ethiopia), and Ministerio de Economía y Competitividad (España)
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Astrophysics::High Energy Astrophysical Phenomena ,Context (language use) ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Luminosity ,high-redshift [Galaxies] ,galaxies: high-redshift ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Luminosity function (astronomy) ,Physics ,[PHYS]Physics [physics] ,010308 nuclear & particles physics ,Star formation ,Astronomy and Astrophysics ,Cosmic variance ,evolution [Galaxies] ,Astrophysics - Astrophysics of Galaxies ,luminosity function [Galaxies] ,Redshift ,Galaxy ,Dark matter halo ,galaxies: luminosity function ,Space and Planetary Science ,mass function ,Mass function ,galaxies: evolution ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
Context. Knowing the exact shape of the ultraviolet (UV) luminosity function (LF) of high-redshift galaxies is important to understand the star formation history of the early Universe. However, the uncertainties, especially at the faint and bright ends of the LFs, remain significant. Aims. In this paper, we study the UV LF of redshift z = 2:5 4.5 galaxies in 2.38 deg of ALHAMBRA data with I ≤ 24. Thanks to the large area covered by ALHAMBRA, we particularly constrain the bright end of the LF. We also calculate the cosmic variance and the corresponding bias values for our sample and derive their host dark matter halo masses. Methods.We have used a novel methodology based on redshift and magnitude probability distribution functions (PDFs). This methodology robustly takes into account the uncertainties due to redshift and magnitude errors, shot noise, and cosmic variance, and models the LF in two dimensions (z; M). Results. We find an excess of bright ∼M∗ galaxies as compared to the studies based on broad-band photometric data. However, our results agree well with the LF of the magnitude-selected spectroscopic VVDS data. We measure high bias values, b ∼ 8 10, that are compatible with the previous measurements considering the redshifts and magnitudes of our galaxies and further reinforce the real high-redshift nature of our bright galaxies. Conclusions. We call into question the shape of the LF at its bright end; is it a double power-law as suggested by the recent broadband photometric studies or rather a brighter Schechter function, as suggested by our multi-filter analysis and the spectroscopic VVDS data.© ESO 2018., K. Viironen acknowledges the >Juan de la Cierva incorporacion> fellowship, IJCI-2014-21960, of the Spanish government. This work has mainly been funded by the FITE (Fondos de Inversiones de Teruel) and the projects AYA2015-66211-C2-1 and AYA2012-30789. We also acknowledge support from the Aragon Government Research Group E103 and support from the Spanish Ministry for Economy and Competitiveness and FEDER funds through grants AYA2010-15081, AYA2010-15169, AYA2010-22111-C03-01, AYA2010-22111-C03-02, AYA2011-29517-C03-01, AYA2012-39620, AYA2013-40611-P, AYA2013-42227-P, AYA2013-43188-P, AYA2013-48623-C2-1, AYA2013-48623-C2-2, ESP2013-48274, AYA2014-58861-C3-1, AYA2016-76682-C3-1-P, Generalitat Valenciana projects Prometeo 2009/064 and PROMETEOII/2014/060, Junta de Andalucia grants TIC114, JA2828, P10-FQM-6444, and Generalitat de Catalunya project SGR-1398. BA has received funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No 656354. MP acknowledges financial supports from the Ethiopian Space Science and Technology Institute (ESSTI) under the Ethiopian Ministry of Science Science and Technology (MoST)
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- 2018
24. The Dark Energy Survey Data Release 1
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M. W. G. Johnson, M. Baumer, Tesla E. Jeltema, Eric H. Neilsen, Peter Nugent, Martin Crocce, S. Hamilton, M. Smith, Antonella Palmese, Nora Shipp, Eli S. Rykoff, F. Nogueira, L. Baruah, Daniel Gruen, Daniel Scolnic, Brian Nord, M. A. G. Maia, Brian Yanny, Matthias Klein, J. Song, R. R. Gupta, Yanxi Zhang, Arya Farahi, J. Carretero, M. March, Basilio X. Santiago, Tamara M. Davis, Shantanu Desai, Gary S. Da Costa, Jochen Weller, T. F. Eifler, Daniel A. Goldstein, J. M. Hislop, Joseph J. Mohr, R. C. Thomas, Erin Sheldon, David Brooks, M. E. C. Swanson, A. Porredon, A. Carnero Rosell, A. Saro, D. W. Gerdes, Xi Chen, Attila Kovács, Eric Morganson, R. C. Wolf, J. P. Dietrich, A. Kremin, T. M. C. Abbott, Richard G. McMahon, Jeremy Mould, J. D. Maloney, Jacobo Asorey, A. Benoit-Lévy, Hiranya V. Peiris, Ofer Lahav, Vinu Vikram, J. Lasker, E. J. Sanchez, B. Flaugher, S. Juneau, Risa H. Wechsler, Ricardo L. C. Ogando, Alistair R. Walker, A. A. Plazas, Ryan J. Foley, M. Carrasco Kind, W. C. Wester, Jennifer L. Marshall, D. L. Burke, Adam Amara, A. Scott, M.L. Sánchez, Jonathan Blazek, C. B. D'Andrea, Marcelle Soares-Santos, R. C. Smith, S. E. Kuhlmann, Ashley J. Ross, Robert C. Nichol, Ben Hoyle, G. Daues, M. Gower, C. J. Miller, M. D. Johnson, Wayne A. Barkhouse, Samuel Hinton, Felipe Menanteau, Kevin Reil, L. Nunes, F. Paz-Chinchón, David J. James, Tenglin Li, Scott Dodelson, Santiago Avila, Ann Elliott, Chihway Chang, T. Kacprzak, G. Tarle, Knut Olsen, R. Das, Ramon Miquel, Lyndsay Old, Juan Garcia-Bellido, E. Bertin, A. Roodman, Tommaso Giannantonio, Carlos E. Cunha, J. Poh, Pablo Fosalba, Enrique Gaztanaga, G. Gutierrez, J. DeRose, J. J. Thaler, Enrique Fernández, Will J. Percival, S. Allam, Paul M. Ricker, A. Pujol, Robert A. Gruendl, V. Scarpine, Andrew B. Pace, R. P. Rollins, K. Honscheid, Timothy A. McKay, Darren L. DePoy, G. Khullar, R. T. Li, Joe Zuntz, Alex Drlica-Wagner, R. Nikutta, Francisco J. Castander, C. Pond, Douglas L. Tucker, Don Petravick, W. G. Hartley, A. K. Vivas, R. Cawthon, Riccardo Campisano, D. A. Finley, D. Brout, Karl Glazebrook, Dragan Huterer, Peter Melchior, Elisabeth Krause, Mark Sullivan, Kyler Kuehn, V. C. Busti, P. Rooney, C. J. Conselice, Huan Lin, Marc Manera, J. Annis, Sebastian Bocquet, A. M. G. Koziol, M. L. Silveira, M. Fitzpatrick, Andrew R. Liddle, Alfredo Zenteno, O. Ballester, Steve Kent, Daniel Thomas, E. Buckley-Geer, Michael Troxel, A. K. Romer, Paul Martini, A. Fausti Neto, Keith Bechtol, C. Davis, J. Gschwend, Gary Bernstein, Hao-Yi Wu, Peter Doel, H. T. Diehl, J. De Vicente, J. P. Marriner, M. S. S. Gill, E. Suchyta, Niall MacCrann, August E. Evrard, Alexandre Refregier, Douglas N. Friedel, Albert Stebbins, M. Banerji, Joshua A. Frieman, I. Sevilla-Noarbe, J. A. Smith, T. McClintock, N. Kuropatkin, L. N. da Costa, Laia Cardiel-Sas, M. Sako, D. L. Hollowood, S. Serrano, David L. Nidever, Marcos Lima, Richard G. Kron, P. Lopez-Reyes, Filipe B. Abdalla, Bhuvnesh Jain, Matthew R. Becker, Flavia Sobreira, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), DES, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), NOAO Data Lab, Abbott, T. M. C., Abdalla, F. B., Allam, S., Amara, A., Annis, J., Asorey, J., Avila, S., Ballester, O., Banerji, M., Barkhouse, W., Baruah, L., Baumer, M., Bechtol, K., Becker, M. R., Benoit-Lévy, A., Bernstein, G. M., Bertin, E., Blazek, J., Bocquet, S., Brooks, D., Brout, Buckley-Geer, E., Burke, D. L., Busti, V., Campisano, R., Cardiel-Sas, L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, X., Conselice, C., Costa, G., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Das, R., Daues, G., Davis, T. M., Davis, C., De Vicente, J., Depoy, D. L., Derose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elliott, A. E., Evrard, A. E., Farahi, A., Fausti Neto, A., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fosalba, P., Friedel, D. N., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gill, M. S. S., Glazebrook, K., Goldstein, D. A., Gower, M., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, R. R., Gutierrez, G., Hamilton, S., Hartley, W. G., Hinton, S. R., Hislop, J. M., Hollowood, D., Honscheid, K., Hoyle, B., Huterer, D., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kacprzak, T., Kent, S., Khullar, G., Klein, M., Kovacs, A., Koziol, A. M. G., Krause, E., Kremin, A., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lasker, J., Li, T. S., Li, R. T., Liddle, A. R., Lima, M., Lin, H., López-Reyes, P., Maccrann, N., Maia, M. A. G., Maloney, J. D., Manera, M., March, M., Marriner, J., Marshall, J. L., Martini, P., Mcclintock, T., Mckay, T., Mcmahon, R. G., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morganson, E., Mould, J., Neilsen, E., Nichol, R. C., Nogueira, F., Nord, B., Nugent, P., Nunes, L., Ogando, R. L. C., Old, L., Pace, A. B., Palmese, A., Paz-Chinchón, F., Peiris, H. V., Percival, W. J., Petravick, D., Plazas, A. A., Poh, J., Pond, C., Porredon, A., Pujol, A., Refregier, A., Reil, K., Ricker, P. M., Rollins, R. P., Romer, A. K., Roodman, A., Rooney, P., Ross, A. J., Rykoff, E. S., Sako, M., Sanchez, M. L., Sanchez, E., Santiago, B., Saro, A., Scarpine, V., Scolnic, D., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shipp, N., Silveira, M. L., Smith, M., Smith, R. C., Smith, J. A., Soares-Santos, M., Sobreira, F., Song, J., Stebbins, A., Suchyta, E., Sullivan, M., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Troxel, M. A., Tucker, D. L., Vikram, V., Vivas, A. K., Walker, A. R., Wechsler, R. H., Weller, J., Wester, W., Wolf, R. C., Wu, H., Yanny, B., Zenteno, A., Zhang, Y., Zuntz, J., Des, Collaboration, Juneau, S., Fitzpatrick, M., Nikutta, R., Nidever, D., Olsen, K., Scott, A., and NOAO Data, Lab
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Astronomical Objects ,catalog ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,techniques: image processing ,Astrophysics ,astronomical databases: miscellaneous ,01 natural sciences ,law.invention ,photometric [techniques] ,techniques: photometric ,law ,Observatory ,Astrophysics - Cosmology and Nongalactic Astrophysic ,010303 astronomy & astrophysics ,[ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det] ,Physics ,image processing [techniques] ,observations [cosmology] ,sky survey ,Astrophysics - Solar and Stellar Astrophysics ,astro-ph.CO ,Astrophysics - Instrumentation and Methods for Astrophysics ,sextractor ,Data release ,observation [cosmology] ,Astrophysics - Cosmology and Nongalactic Astrophysics ,astro-ph.SR ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Aperture ,astro-ph.GA ,FOS: Physical sciences ,Astronomy & Astrophysics ,miscellaneou [astronomical databases] ,Telescope ,surveys ,Astrophysics - Astrophysics of Galaxie ,0103 physical sciences ,survey ,Astronomical And Space Sciences ,[PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det] ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Solar and Stellar Astrophysics (astro-ph.SR) ,Physical Chemistry (Incl. Structural) ,010308 nuclear & particles physics ,Organic Chemistry ,representations ,Astronomy and Astrophysics ,miscellaneous [astronomical databases] ,angular masks ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Data set ,catalogs ,cosmology: observations ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Dark energy ,Astrophysics - Instrumentation and Methods for Astrophysic ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,astro-ph.IM - Abstract
We describe the first public data release of the Dark Energy Survey, DES DR1, consisting of reduced single epoch images, coadded images, coadded source catalogs, and associated products and services assembled over the first three years of DES science operations. DES DR1 is based on optical/near-infrared imaging from 345 distinct nights (August 2013 to February 2016) by the Dark Energy Camera mounted on the 4-m Blanco telescope at Cerro Tololo Inter-American Observatory in Chile. We release data from the DES wide-area survey covering ~5,000 sq. deg. of the southern Galactic cap in five broad photometric bands, grizY. DES DR1 has a median delivered point-spread function of g = 1.12, r = 0.96, i = 0.88, z = 0.84, and Y = 0.90 arcsec FWHM, a photometric precision of < 1% in all bands, and an astrometric precision of 151 mas. The median coadded catalog depth for a 1.95" diameter aperture at S/N = 10 is g = 24.33, r = 24.08, i = 23.44, z = 22.69, and Y = 21.44 mag. DES DR1 includes nearly 400M distinct astronomical objects detected in ~10,000 coadd tiles of size 0.534 sq. deg. produced from ~39,000 individual exposures. Benchmark galaxy and stellar samples contain ~310M and ~ 80M objects, respectively, following a basic object quality selection. These data are accessible through a range of interfaces, including query web clients, image cutout servers, jupyter notebooks, and an interactive coadd image visualization tool. DES DR1 constitutes the largest photometric data set to date at the achieved depth and photometric precision., 30 pages, 20 Figures. Release page found at this url https://des.ncsa.illinois.edu/releases/dr1
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- 2018
25. The PAU Survey: A Forward Modeling Approach for Narrow-band Imaging
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Pau Tallada, Juan de Vicente, Alexandre Refregier, C. Padilla, Santiago Serrano, J. Carretero, Nadia Tonello, A. Alarcon, E. J. Sanchez, Lorenza Della Bruna, Jörg Herbel, Francisco J. Castander, Enrique Gaztanaga, Enrique Fernández, Luca Tortorelli, Martin Folger, Juan Garcia-Bellido, Lee Stothert, Adam Amara, Ramon Miquel, and Martin Eriksen
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Physics ,education.field_of_study ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Pixel ,010308 nuclear & particles physics ,Population ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Residual ,Astrophysics - Astrophysics of Galaxies ,01 natural sciences ,Galaxy ,Redshift ,Photometry (optics) ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Principal component analysis ,Statistical physics ,education ,010303 astronomy & astrophysics ,Weak gravitational lensing ,galaxy surveys ,dark energy experiments ,dark matter experiments ,redshift surveys ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Weak gravitational lensing is a powerful probe of the dark sector, once measurement systematic errors can be controlled. In Refregier & Amara (2014), a calibration method based on forward modeling, called MCCL, was proposed. This relies on fast image simulations (e.g., UFig; Berge et al. 2013) that capture the key features of galaxy populations and measurement effects. The MCCL approach has been used in Herbel et al. (2017) to determine the redshift distribution of cosmological galaxy samples and, in the process, the authors derived a model for the galaxy population mainly based on broad-band photometry. Here, we test this model by forward modeling the 40 narrow-band photometry given by the novel PAU Survey (PAUS). For this purpose, we apply the same forced photometric pipeline on data and simulations using Source Extractor (Bertin & Arnouts 1996). The image simulation scheme performance is assessed at the image and at the catalogues level. We find good agreement for the distribution of pixel values, the magnitudes, in the magnitude-size relation and the interband correlations. A principal component analysis is then performed, in order to derive a global comparison of the narrow-band photometry between the data and the simulations. We use a `mixing' matrix to quantify the agreement between the observed and simulated sets of Principal Components (PCs). We find good agreement, especially for the first three most significant PCs. We also compare the coefficients of the PCs decomposition. While there are slight differences for some coefficients, we find that the distributions are in good agreement. Together, our results show that the galaxy population model derived from broad-band photometry is in good overall agreement with the PAUS data. This offers good prospect for incorporating spectral information to the galaxy model by adjusting it to the PAUS narrow-band data using forward modeling., Submitted to JCAP, 28 pages, 15 figures, 3 appendices
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- 2018
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26. DES Science Portal: Computing Photometric Redshifts
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Paulo S. Pellegrini, J. Calcino, David J. James, E. Suchyta, August E. Evrard, Pablo Fosalba, Antonella Palmese, G. Tarle, C. Adean, Filipe B. Abdalla, Geraint F. Lewis, Tamara M. Davis, Karl Glazebrook, Douglas L. Tucker, C. Lidman, Kyler Kuehn, Marcos Lima, J. Asorey, David J. Brooks, C. Singulani, Daniela Carollo, I. Sevilla-Noarbe, J. Annis, M. Carrasco Kind, A. C. Rossel, C. B. D'Andrea, N. Kuropatkin, M. E. C. Swanson, Francisco J. Castander, L. N. da Costa, Jennifer L. Marshall, Brad E. Tucker, Flavia Sobreira, T. M. C. Abbott, Peter Melchior, D. L. Hollowood, Michel Aguena, M. Smith, V. Scarpine, A. A. Plazas, E. J. Sanchez, M. A. G. Maia, Basilio X. Santiago, Alistair R. Walker, Ricardo L. C. Ogando, I. Sadeh, S. Allam, Robert A. Gruendl, Ben Hoyle, D. W. Gerdes, Joshua A. Frieman, C. Benoist, Riccardo Campisano, Angelo Fausti Neto, J. De Vicente, S. A. Uddin, Huan Lin, K. Honscheid, Ofer Lahav, W. G. Hartley, R. H. Schindler, J. K. Hoormann, Edward Macaulay, Samuel Hinton, G. Gutierrez, N. E. Sommer, Sachin N. Desai, J. Gschwend, Ramon Miquel, Anais Möller, Juan Garcia-Bellido, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
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Data interface ,photometry ,Computer science ,FOS: Physical sciences ,Context (language use) ,computer.software_genre ,01 natural sciences ,Astronomical data bases: surveys ,Scientific analysis ,Galaxies: distances and redshifts ,surveys ,Methods: data analysis ,0103 physical sciences ,distances and redshifts, statistics [Galaxies] ,Astronomical databases: catalogs ,[PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det] ,data analysis [Methods] ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,STFC ,010308 nuclear & particles physics ,RCUK ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,DES ,Redshift ,Computer Science Applications ,Workflow ,Space and Planetary Science ,statistics ,Astrophysics of Galaxies (astro-ph.GA) ,ddc:520 ,Data mining ,catalogs, surveys [Astronomical databases] ,Astrophysics - Instrumentation and Methods for Astrophysics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,computer - Abstract
Astronomy and computing 25, 58-80 (2018). doi:10.1016/j.ascom.2018.08.008, A significant challenge facing photometric surveys for cosmological purposes is the need to produce reliable redshift estimates. The estimation of photometric redshifts (photo-s) has been consolidated as the standard strategy to bypass the high production costs and incompleteness of spectroscopic redshift samples. Training-based photo- methods require the preparation of a high-quality list of spectroscopic redshifts, which needs to be constantly updated. The photo- training, validation, and estimation must be performed in a consistent and reproducible way in order to accomplish the scientific requirements. To meet this purpose, we developed an integrated web-based data interface that not only provides the framework to carry out the above steps in a systematic way, enabling the ease testing and comparison of different algorithms, but also addresses the processing requirements by parallelizing the calculation in a transparent way for the user. This framework called the Science Portal (hereafter Portal) was developed in the context the Dark Energy Survey (DES) to facilitate scientific analysis. In this paper, we show how the Portal can provide a reliable environment to access vast datasets, provide validation algorithms and metrics, even in the case of multiple photo-s methods. It is possible to maintain the provenance between the steps of a chain of workflows while ensuring reproducibility of the results. We illustrate how the Portal can be used to provide photo- estimates using the DES first year (Y1A1) data. While the DES collaboration is still developing techniques to obtain more precise photo-s, having a structured framework like the one presented here is critical for the systematic vetting of DES algorithmic improvements and the consistent production of photo-zs in future DES releases., Published by Elsevier, Amsterdam [u.a.]
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- 2018
27. Core or Cusps: The Central Dark Matter Profile of a Strong Lensing Cluster with a Bright Central Image at Redshift 1
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G. Gutierrez, Tim Eifler, Ramon Miquel, Daniel A. Goldstein, Thomas E. Collett, V. Scarpine, Shantanu Desai, Douglas L. Tucker, Kyler Kuehn, Mathew Smith, Xan Morice-Atkinson, Andrs A. Plazas, Chris B. D'Andrea, Alistair R. Walker, Peter Doel, D. L. Burke, David Bacon, B. Flaugher, David Brooks, David J. James, Nikolay Kuropatkin, I. Sevilla-Noarbe, E. Suchyta, Rafe Schindler, Brian Nord, Anupreeta More, Simon Birrer, Luiz N. da Costa, H. Thomas Diehl, Josh Frieman, S. Allam, Aurlien Benoit-Levy, Marcos Lima, J. Gschwend, Flavia Sobreira, Casey Papovich, Jennifer L. Marshal, Peter Melchior, E. Buckley-Geer, James Annis, K. Romer, Matias Carrasco Kind, M. March, Molly E. C. Swanson, Huan Lin, Paul Martini, Michael Schubnell, Adam Amara, Nicolas Tessore, Daniel Gruen, D. W. Gerdes, Robert C. Nichol, Francisco J. Castander, Marcio A. G. Maia, Gregory Tarle, Eli S. Rykoff, T. M. C. Abbott, Ofer Lahav, E. J. Sanchez, Tenglin Li, Steve Kuhlmann, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
- Subjects
galaxies: clusters: individual ,Cold dark matter ,Einstein ring ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,clusters: individual (SPT-CLJ2011-5228) [galaxies] ,Dark matter ,galaxies: halos ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,01 natural sciences ,Physical Chemistry ,Atomic ,dark matter ,symbols.namesake ,Particle and Plasma Physics ,0103 physical sciences ,Nuclear ,010306 general physics ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,Mass distribution ,clusters: individual [galaxies] ,Molecular ,gravitational lensing: strong ,Astronomy and Astrophysics ,Radius ,Redshift ,halos [galaxies] ,Gravitational lens ,Space and Planetary Science ,strong [gravitational lensing] ,symbols ,Dark energy ,Biomedical Imaging ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astronomical and Space Sciences ,Physical Chemistry (incl. Structural) - Abstract
International audience; We report on SPT-CLJ2011-5228, a giant system of arcs created by a cluster at z = 1.06. The arc system is notable for the presence of a bright central image. The source is a Lyman break galaxy at z ( )s( ) = 2.39 and the mass enclosed within the Einstein ring of radius 14 arcsec is $\sim {10}^{14.2}\ {M}_{\odot }$. We perform a full reconstruction of the light profile of the lensed images to precisely infer the parameters of the mass distribution. The brightness of the central image demands that the central total density profile of the lens be shallow. By fitting the dark matter as a generalized Navarro–Frenk–White profile—with a free parameter for the inner density slope—we find that the break radius is ${270}_{-76}^{+48}$ kpc, and that the inner density falls with radius to the power −0.38 ± 0.04 at 68% confidence. Such a shallow profile is in strong tension with our understanding of relaxed cold dark matter halos, dark matter-only simulations predict that the inner density should fall as ${r}^{-1}$. The tension can be alleviated if this cluster is in fact a merger, a two-halo model can also reconstruct the data, with both clumps (density varying as ${r}^{-0.8}$ and ${r}^{-1.0}$) much more consistent with predictions from dark matter-only simulations. At the resolution of our Dark Energy Survey imaging, we are unable to choose between these two models, but we make predictions for forthcoming Hubble Space Telescope imaging that will decisively distinguish between them.
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- 2017
28. The Complete Calibration of the Color-Redshift Relation (C3R2) Survey: Survey Overview and Data Release 1
- Author
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Daniel Stern, Daniel Masters, Jason Rhodes, Judy Cohen, Stéphane Paltani, Peter Capak, and Francisco J. Castander
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Gran Telescopio Canarias ,Physics ,Very Large Telescope ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astronomy ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,01 natural sciences ,Redshift ,Galaxy ,Cosmology ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,0103 physical sciences ,Dark energy ,010303 astronomy & astrophysics ,Weak gravitational lensing ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Photometric redshift - Abstract
A key goal of the Stage IV dark energy experiments Euclid, LSST and WFIRST is to measure the growth of structure with cosmic time from weak lensing analysis over large regions of the sky. Weak lensing cosmology will be challenging: in addition to highly accurate galaxy shape measurements, statistically robust and accurate photometric redshift (photo-z) estimates for billions of faint galaxies will be needed in order to reconstruct the three-dimensional matter distribution. Here we present an overview of and initial results from the Complete Calibration of the Color-Redshift Relation (C3R2) survey, designed specifically to calibrate the empirical galaxy color-redshift relation to the Euclid depth. These redshifts will also be important for the calibrations of LSST and WFIRST. The C3R2 survey is obtaining multiplexed observations with Keck (DEIMOS, LRIS, and MOSFIRE), the Gran Telescopio Canarias (GTC; OSIRIS), and the Very Large Telescope (VLT; FORS2 and KMOS) of a targeted sample of galaxies most important for the redshift calibration. We focus spectroscopic efforts on under-sampled regions of galaxy color space identified in previous work in order to minimize the number of spectroscopic redshifts needed to map the color-redshift relation to the required accuracy. Here we present the C3R2 survey strategy and initial results, including the 1283 high confidence redshifts obtained in the 2016A semester and released as Data Release 1., Comment: Accepted to ApJ. 11 pages, 5 figures. Redshifts can be found at http://c3r2.ipac.caltech.edu/c3r2_DR1_mrt.txt
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- 2017
29. nIFTy Cosmology: the clustering consistency of galaxy formation models
- Author
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Peter A. Thomas, Frazer R. Pearce, A. Cattaneo, Sofía A. Cora, Michaela Hirschmann, Arnau Pujol, Fabio Fontanot, Nelson D. Padilla, Chris Power, John C. Helly, Daniel Cunnama, Andrew J. Benson, Richard G. Bower, Darren J. Croton, Ignacio D Gargiulo, Jeremy Blaizot, Ramin A. Skibba, Alexander Knebe, Bruno M. B. Henriques, Violeta Gonzalez-Perez, Gary A. Mamon, Julian Onions, Juan Garcia-Bellido, Pierluigi Monaco, Sukyoung K. Yi, Cristian A Vega-Martínez, Pascal J. Elahi, J. Carretero, Julien Devriendt, Chaichalit Srisawat, Edouard Tollet, Enrique Gaztanaga, Jaehyun Lee, Weiguang Cui, Rachel S. Somerville, Andreea S. Font, Francisco J. Castander, Gabriella De Lucia, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) ( DAP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Centre de Recherche Astrophysique de Lyon ( CRAL ), École normale supérieure - Lyon ( ENS Lyon ) -Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Galaxies, Etoiles, Physique, Instrumentation ( GEPI ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Pujol, and Skibba, A., and Gazta\~naga, R. ~. A., and Benson, E., and Blaizot, A., and Bower, J., and Carretero, R., and Castander, J., and Cattaneo, F. ~. J., and Cora, A., and Croton, S. ~. A., and Cui, D. ~. J., and Cunnama, W., and De Lucia, D., and Devriendt, G., and Elahi, J. ~. E., and Font, P. ~. J., and Fontanot, A., and Garcia-Bellido, F., and Gargiulo, J., and Gonzalez-Perez, I. ~. D., and Helly, V., and Henriques, J., and Hirschmann, B. ~. M. ~. B., and Knebe, M., and Lee, A., and Mamon, J., Monaco, P., Onions, And, and Padilla, J., and Pearce, N. ~. D., and Power, F. ~. R., and Somerville, C., and Srisawat, R. ~. S., and Thomas, C., and Tollet, P. ~. A., and Vega-Mart\'\inez, E., and Yi, C. ~. A., and ~. K., S.
- Subjects
Ciencias Astronómicas ,Cold dark matter ,Ciencias Físicas ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,Astrophysics ,ST/L000652/1 ,01 natural sciences ,purl.org/becyt/ford/1 [https] ,cosmology: theory ,Satellite galaxy ,010303 astronomy & astrophysics ,QC ,QB ,Physics ,theory [cosmology] ,haloe [galaxies] ,haloes [galaxies] ,astro-ph.CO ,Halo ,CIENCIAS NATURALES Y EXACTAS ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Cosmology and Gravitation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,astro-ph.GA ,Astrophysics::High Energy Astrophysical Phenomena ,Dark matter ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Halo occupation distribution ,numerical ,galaxies: haloes ,cosmology: theory [methods] ,methods: numerical ,0103 physical sciences ,Galaxy formation and evolution ,Cluster analysis ,STFC ,Astrophysics::Galaxy Astrophysics ,010308 nuclear & particles physics ,RCUK ,Astronomy ,numerical [methods] ,Astronomy and Astrophysics ,purl.org/becyt/ford/1.3 [https] ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Astronomía ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
We present a clustering comparison of 12 galaxy formation models [including semi-analytic models (SAMs) and halo occupation distribution (HOD) models] all run on halo catalogues and merger trees extracted from a single Λ cold dark matter N-body simulation. We compare the results of the measurements of the mean halo occupation numbers, the radial distribution of galaxies in haloes and the two-point correlation functions (2PCF). We also study the implications of the different treatments of orphan (galaxies not assigned to any dark matter subhalo) and non-orphan galaxies in these measurements. Our main result is that the galaxy formation models generally agree in their clustering predictions but they disagree significantly between HOD and SAMs for the orphan satellites. Although there is a very good agreement between the models on the 2PCF of central galaxies, the scatter between the models when orphan satellites are included can be larger than a factor of 2 for scales smaller than 1 h(−1) Mpc. We also show that galaxy formation models that do not include orphan satellite galaxies have a significantly lower 2PCF on small scales, consistent with previous studies. Finally, we show that the 2PCF of orphan satellites is remarkably different between SAMs and HOD models. Orphan satellites in SAMs present a higher clustering than in HOD models because they tend to occupy more massive haloes. We conclude that orphan satellites have an important role on galaxy clustering and they are the main cause of the differences in the clustering between HOD models and SAMs., Monthly Notices of the Royal Astronomical Society, 469 (1), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711
- Published
- 2017
30. Inference from the small scales of cosmic shear with current and future Dark Energy Survey data
- Author
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G. Gutierrez, Shantanu Desai, Marcelle Soares-Santos, T. Kacprzak, Robert Armstrong, Marcos Lima, Adam Amara, J. Annis, David J. James, Erin Sheldon, David Brooks, I. Sevilla-Noarbe, Tim Eifler, A. Benoit-Lévy, Kyler Kuehn, Felipe Menanteau, Pablo Fosalba, D. L. Burke, Elisabeth Krause, Risa H. Wechsler, Jennifer L. Marshall, L. N. da Costa, Gregory Tarle, J. Aleksić, Claudio Bruderer, S. Allam, Eli S. Rykoff, Daniel Gruen, Robert A. Gruendl, E. Suchyta, August E. Evrard, V. Vikram, Ramon Miquel, A. K. Romer, Alexandre Refregier, Martin Crocce, V. Scarpine, Daniel Thomas, M. E. C. Swanson, D. W. Gerdes, A. Carnero Rosell, E. M. Huff, M. Jarvis, Dragan Huterer, Peter Doel, Francisco J. Castander, M. Carrasco Kind, K. Honscheid, H. T. Diehl, Peter Melchior, Niall MacCrann, A. A. Plazas, J. Carretero, Daniel A. Goldstein, J. P. Dietrich, B. Flaugher, Nikolay Kuropatkin, Sarah Bridle, Scott Dodelson, Chihway Chang, Carlos E. Cunha, T. M. C. Abbott, E. J. Sanchez, Joe Zuntz, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
- Subjects
Cosmology and Gravitation ,Active galactic nucleus ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,gravitational lensing: weak ,weak [gravitational lensing] ,0103 physical sciences ,Galaxy formation and evolution ,010303 astronomy & astrophysics ,weak ,Large-scale structure of Universe [Gravitational lensing] ,Galaxy cluster ,Weak gravitational lensing ,STFC ,QB ,Physics ,COSMIC cancer database ,010308 nuclear & particles physics ,Astronomy ,RCUK ,Astronomy and Astrophysics ,Galaxy ,Space and Planetary Science ,Dark energy ,astro-ph.CO ,Halo ,large-scale structure of Universe ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Monthly Notices of the Royal Astronomical Society, 465 (3), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711
- Published
- 2017
31. DES15E2mlf: a spectroscopically confirmed superluminous supernova that exploded 3.5 Gyr after the big bang
- Author
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Peter Nugent, C. Lidman, Eve Kovacs, A. K. Romer, E. Buckley-Geer, Juan Garcia-Bellido, Kyler Kuehn, Flavia Sobreira, M. A. G. Maia, Paul Martini, David J. James, A. Papadopoulos, R. C. Smith, M. E. C. Swanson, Alistair R. Walker, Lluís Galbany, A. Benoit-Lévy, G. Gutierrez, C. B. D'Andrea, Ryan J. Foley, Ofer Lahav, Michael Schubnell, Yen-Chen Pan, J. Annis, Elisabeth Krause, M. March, Keith Bechtol, Jennifer L. Marshall, V. Scarpine, Shantanu Desai, Mathew Smith, Joshua A. Frieman, A. Carnero Rosell, I. Sevilla-Noarbe, E. Suchyta, A. A. Plazas, Ramon Miquel, Mark Sullivan, Carlos E. Cunha, F. B. Abdalla, N. Kuropatkin, Matt J. Jarvis, Tim Eifler, Santiago González-Gaitán, L. N. da Costa, T. M. C. Abbott, David J. Brooks, M. Sako, E. J. Sanchez, Richard Kessler, D. L. Burke, Marcos Lima, J. Gschwend, Peter Doel, Robert A. Gruendl, H. T. Diehl, J. Carretero, Daniel A. Goldstein, R. C. Thomas, Daniel Gruen, M. Carrasco Kind, Robert C. Nichol, D. A. Finley, A. G. Kim, Francisco J. Castander, B. Flaugher, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
- Subjects
astro-ph.SR ,Stellar mass ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,astro-ph.GA ,individual: DES15E2mlf [supernovae] ,FOS: Physical sciences ,Astrophysics ,Astronomy & Astrophysics ,medicine.disease_cause ,01 natural sciences ,supernovae: general ,0103 physical sciences ,medicine ,Spectroscopy ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,supernovae: individual: DES15E2mlf ,QB ,Physics ,010308 nuclear & particles physics ,Astronomy ,Astronomy and Astrophysics ,Light curve ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Galaxy ,Supernova ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Dark energy ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,general [supernovae] ,Ultraviolet ,Astronomical and Space Sciences - Abstract
We present the Dark Energy Survey (DES) discovery of DES15E2mlf, the most distant superluminous supernova (SLSN) spectroscopically confirmed to date. The light curves and Gemini spectroscopy of DES15E2mlf indicate that it is a Type I superluminous supernova (SLSN-I) at z = 1.861 (a lookback time of ~10 Gyr) and peaking at M_AB = -22.3 +/- 0.1 mag. Given the high redshift, our data probe the rest-frame ultraviolet (1400-3500 A) properties of the SN, finding velocity of the C III feature changes by ~5600 km/s over 14 days around maximum light. We find the host galaxy of DES15E2mlf has a stellar mass of 3.5^+3.6_-2.4 x 10^9 M_sun, which is more massive than the typical SLSN-I host galaxy., MNRAS in press
- Published
- 2017
32. Precise photometric redshifts with a narrow-band filter set: the PAU survey at the William Herschel Telescope
- Author
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Carles Sanchez, Enrique Gaztanaga, P. Martí, Martin Eriksen, Ramon Miquel, and Francisco J. Castander
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,FOS: Physical sciences ,Astronomy ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Redshift survey ,Bin ,Redshift ,Galaxy ,Matrix (mathematics) ,Wavelength ,Space and Planetary Science ,Filter (video) ,William Herschel Telescope ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The Physics of the Accelerating Universe (PAU) survey at the William Herschel Telescope (WHT) will use a new optical camera (PAUCam) with a large set of narrow-band filters to perform a photometric galaxy survey with a quasi-spectroscopic redshift precision of \sigma(z)/(1 + z) ~ 0.0035 and map the large-scale structure of the universe in three dimensions up to i_AB < 22.5-23.0. In this paper we present a detailed photo-z performance study using photometric simulations for 40 equally-spaced 12.5-nm-wide (FWHM) filters with a ~25% overlap and spanning the wavelength range from 450 nm to 850 nm, together with a ugrizY broad-band filter system. We then present the migration matrix r_ij, containing the probability that a galaxy in a true redshift bin j is measured in a photo-z bin i, and study its effect on the determination of galaxy auto- and cross-correlations. Finally, we also study the impact on the photo-z performance of small variations of the filter set in terms of width, wavelength coverage, etc., and find a broad region where slightly modified filter sets provide similar results, with the original set being close to optimal., Comment: Accepted for publication in MNRAS. 19 pages, 18 figures, 6 tables
- Published
- 2014
33. Joint analysis of galaxy-galaxy lensing and galaxy clustering: methodology and forecasts for dark energy survey
- Author
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K. Honscheid, Christopher J. Miller, E. S. Rykoff, Natalie A. Roe, Jennifer L. Marshall, D. A. Finley, Shantanu Desai, Carles Sanchez, Enrique Gaztanaga, J. Carretero, A. Benoit-Lévy, E. Bertin, A. Carnero Rosell, Vinu Vikram, E. Buckley-Geer, F. B. Abdalla, Tim Eifler, Daniel Gruen, J. Zuntz, Elisabeth Krause, V. Scarpine, G. Gutierrez, M. Carrasco Kind, Ricardo L. C. Ogando, P. Fosalba, Alistair R. Walker, Matthew R. Becker, Flavia Sobreira, M. Schubnell, Robert C. Nichol, J. J. Thaler, Youngsoo Park, Sarah Bridle, Scott Dodelson, D. L. Burke, Marcelle Soares-Santos, D. W. Gerdes, Martin Crocce, Ramon Miquel, Jochen Weller, Francisco J. Castander, T. M. C. Abbott, David Brooks, M. E. C. Swanson, E. Fernandez, A. A. Plazas, E. J. Sanchez, Adam Amara, S. Allam, Robert A. Gruendl, Gregory Tarle, David J. James, Peter Doel, E. Suchyta, B. Flaugher, Darren L. DePoy, Steve Kent, Risa H. Wechsler, Eduardo Rozo, Nikolay Kuropatkin, A. K. Romer, Bhuvnesh Jain, A. Fausti Neto, I. Sevilla-Noarbe, J. P. Dietrich, L. N. da Costa, Kyler Kuehn, Joseph Clampitt, Marcos Lima, Peter Melchior, and M. A. G. Maia
- Subjects
Physics ,Observational error ,010308 nuclear & particles physics ,AST-1138766 ,RCUK ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Halo occupation distribution ,Cosmology ,Galaxy ,0103 physical sciences ,Dark energy ,astro-ph.CO ,Cluster analysis ,dark energy ,010303 astronomy & astrophysics ,cosmology ,uploaded-in-3-months-elsewhere ,Weak gravitational lensing ,STFC ,Astrophysics::Galaxy Astrophysics ,Photometric redshift ,QB - Abstract
The joint analysis of galaxy-galaxy lensing and galaxy clustering is a promising method for inferring the growth function of large scale structure. This analysis will be carried out on data from the Dark Energy Survey (DES), with its measurements of both the distribution of galaxies and the tangential shears of background galaxies induced by these foreground lenses. We develop a practical approach to modeling the assumptions and systematic effects affecting small scale lensing, which provides halo masses, and large scale galaxy clustering. Introducing parameters that characterize the halo occupation distribution (HOD), photometric redshift uncertainties, and shear measurement errors, we study how external priors on different subsets of these parameters affect our growth constraints. Degeneracies within the HOD model, as well as between the HOD and the growth function, are identified as the dominant source of complication, with other systematic effects sub-dominant. The impact of HOD parameters and their degeneracies necessitate the detailed joint modeling of the galaxy sample that we employ. We conclude that DES data will provide powerful constraints on the evolution of structure growth in the universe, conservatively/optimistically constraining the growth function to 7.9%/4.8% with its first-year data that covered over 1000 square degrees, and to 3.9%/2.3% with its full five-year data that will survey 5000 square degrees, including both statistical and systematic uncertainties.
- Published
- 2016
34. redMaGiC: selecting luminous red galaxies from the DES Science Verification data
- Author
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Alistair R. Walker, Marcelle Soares-Santos, Flavia Sobreira, Peter Doel, Martin Crocce, Ricardo L. C. Ogando, H. T. Diehl, Enrique Gaztanaga, Vinu Vikram, Eli S. Rykoff, M. March, Basilio X. Santiago, M. Carrasco Kind, Robert C. Nichol, M. Jarvis, Ben Hoyle, J. J. Thaler, A. H. Bauer, T. M. C. Abbott, Hiranya V. Peiris, D. L. Burke, E. Bertin, C. Davis, E. J. Sanchez, C. Bonnett, Shantanu Desai, I. Sevilla-Noarbe, A. Benoit-Lévy, Syed Uddin, Daniela Carollo, A. A. Plazas, Gary Bernstein, Brian Nord, Marcio A. G. Maia, Diego Capozzi, Peter Melchior, Carlos E. Cunha, Robert A. Gruendl, David Brooks, M. E. C. Swanson, P. Fosalba, C. Lidman, Ofer Lahav, Alexandra Abate, Darren L. DePoy, A. Carnero Rosell, L. N. da Costa, Eduardo Rozo, David J. James, Kyler Kuehn, Ramon Miquel, Daniel Thomas, E. Buckley-Geer, Tim Eifler, Karl Glazebrook, W. C. Wester, Manda Banerji, Risa H. Wechsler, R. C. Smith, J. Carretero, K. Honscheid, Tamara M. Davis, A. K. Romer, Paul Martini, B. Flaugher, C. B. D'Andrea, A. Fausti Neto, J. P. Dietrich, Nikolay Kuropatkin, A. Roodman, M. J. Childress, Joshua A. Frieman, C. R. O'Neill, E. Suchyta, August E. Evrard, Joseph J. Mohr, Michael Schubnell, M. Sako, A. G. Kim, Marcos Lima, Boris Leistedt, Francisco J. Castander, Y. Zhang, F. B. Abdalla, Daniel Gruen, D. W. Gerdes, and C. J. Miller
- Subjects
Cosmology and Gravitation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Gaussian ,media_common.quotation_subject ,astro-ph.GA ,statistical [methods] ,Extrapolation ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,01 natural sciences ,photometric [techniques] ,symbols.namesake ,0103 physical sciences ,010303 astronomy & astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,STFC ,Astrophysics::Galaxy Astrophysics ,Photometric redshift ,media_common ,QB ,Physics ,010308 nuclear & particles physics ,Sigma ,Astronomy ,RCUK ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Galaxy ,Space and Planetary Science ,Sky ,Astrophysics of Galaxies (astro-ph.GA) ,Outlier ,symbols ,astro-ph.CO ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astronomical and Space Sciences ,Astrophysics - Cosmology and Nongalactic Astrophysics ,general [galaxies] ,astro-ph.IM - Abstract
We introduce redMaGiC, an automated algorithm for selecting Luminous Red Galaxies (LRGs). The algorithm was specifically developed to minimize photometric redshift uncertainties in photometric large-scale structure studies. redMaGiC achieves this by self-training the color-cuts necessary to produce a luminosity-thresholded LRG sample of constant comoving density. We demonstrate that redMaGiC photozs are very nearly as accurate as the best machine-learning based methods, yet they require minimal spectroscopic training, do not suffer from extrapolation biases, and are very nearly Gaussian. We apply our algorithm to Dark Energy Survey (DES) Science Verification (SV) data to produce a redMaGiC catalog sampling the redshift range $z\in[0.2,0.8]$. Our fiducial sample has a comoving space density of $10^{-3}\ (h^{-1} Mpc)^{-3}$, and a median photoz bias ($z_{spec}-z_{photo}$) and scatter $(\sigma_z/(1+z))$ of 0.005 and 0.017 respectively. The corresponding $5\sigma$ outlier fraction is 1.4%. We also test our algorithm with Sloan Digital Sky Survey (SDSS) Data Release 8 (DR8) and Stripe 82 data, and discuss how spectroscopic training can be used to control photoz biases at the 0.1% level., Comment: comments welcome
- Published
- 2016
35. ProtoDESI: risk reduction experiment for the Dark Energy Spectroscopic Instrument
- Author
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K. Honscheid, G. Tarle, Arjun Dey, Irena Gershkovich, Michael Schubnell, David Rabinowitz, Robert Marshall, Parker Fagrelius, C. Baltay, Robert Besuner, Joseph H. Silber, Stephen B. H. Kent, Kevin Reil, W. Emmet, Dick Joyce, Ronald G. Probst, Ann Elliott, E. Buckley-Geer, Chris Bebek, Santiago Serrano, B. Flaugher, David Sprayberry, Francisco J. Castander, and David J. Schlegel
- Subjects
Physics ,Photometry (optics) ,Optics ,business.industry ,Dark energy ,Astrophysics ,Baryon acoustic oscillations ,Spectroscopy ,business - Published
- 2016
36. Characterization and performance of PAUCam filters
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Ricard Casas, J. Gaweda, C. Padilla, I. Sevilla Noarbe, M. Lamensans, Laia Cardiel-Sas, Carlos Díaz, S. Jiménez, F. J. Rodriguez, E. J. Sanchez, Francisco J. Castander, and J. Jiménez Rojas
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Physics ,Large field of view ,010308 nuclear & particles physics ,business.industry ,Operation temperature ,01 natural sciences ,Characterization (materials science) ,Filter system ,Optics ,Cardinal point ,0103 physical sciences ,William Herschel Telescope ,Focus (optics) ,business ,010303 astronomy & astrophysics ,Beam (structure) - Abstract
PAUCam is a large field of view camera designed to exploit the field delivered by the prime focus corrector of the William Herschel Telescope, at the Observatorio del Roque de los Muchachos. One of the new features of this camera is its filter system, placed within a few millimeters of the focal plane using eleven trays containing 40 narrow band and 6 broad band filters, working in vacuum at an operational temperature of 250K and in a focalized beam. In this contribution, we describe the performance of these filters both in the characterization tests at the laboratory.
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- 2016
37. The PAU camera carbon fiber cryostat and filter interchange system
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Laia Cardiel-Sas, Cristobal Padilla, Ferran Grañena, O. Ballester, Luis Lopez, Ester Majà, and Francisco J. Castander
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Physics ,Cryostat ,Galactic astronomy ,010308 nuclear & particles physics ,business.industry ,Carbon fibers ,Mechanical engineering ,01 natural sciences ,Large sample ,Optics ,Filter (video) ,visual_art ,0103 physical sciences ,William Herschel Telescope ,visual_art.visual_art_medium ,business ,010303 astronomy & astrophysics - Abstract
This paper describes the engineering and mechanical considerations in the design and construction of a carbon fiber containment vessel for a photometric camera. The camera is intended for installation on the 4 m William Herschel Telescope, located in Palma, Spain. The scientific objective of the camera system is to measure red-shifts of a large sample of galaxies using the photometric technique. The paper is broken down into sections, divided by the principal engineering challenges of the project; the carbon fiber vacuum vessel, the cooling systems and the precision movement systems.
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- 2016
38. The Dark Energy Survey: more than dark energy – an overview
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V. Scarpine, Peter Doel, Alex Drlica-Wagner, M. Carrasco-Kind, Eric H. Neilsen, H. T. Diehl, William G. Hartley, Martin Crocce, David Bacon, Jochen Weller, Huan Lin, Michael Schubnell, L. Clerkin, Daniel Thomas, E. Buckley-Geer, L. Whiteway, A. K. Romer, Paul Martini, J. Fabbri, Marcio A. G. Maia, Donnacha Kirk, Alistair R. Walker, Marcelle Soares-Santos, C. Bonnett, Brian Yanny, T. M. C. Abbott, Antonella Palmese, Erin Sheldon, David Brooks, M. E. C. Swanson, Hiranya V. Peiris, D. L. Burke, Shantanu Desai, E. J. Sanchez, Mathew Smith, Stephanie Jouvel, A. Benoit-Lévy, Vinu Vikram, Ryan J. Foley, I. Sadeh, A. L. King, Joe Zuntz, Jennifer L. Marshall, Ashley J. Ross, S. Allam, Marcella Carollo, Robert A. Gruendl, H. Wilcox, C. B. D'Andrea, J. Etherington, F. B. Abdalla, Bhuvnesh Jain, Xan Morice-Atkinson, Tesla E. Jeltema, F. Ostrovski, David J. James, Yanming Zhang, Christopher J. Miller, Ramon Miquel, A. Carnero-Rosell, C. Sánchez, John Peoples, B. Flaugher, Pablo Fosalba, E. Bertin, Ofer Lahav, Keith Bechtol, Maayane T. Soumagnac, Will J. Percival, Thomas E. Collett, Daniel Gruen, Nikolay Kuropatkin, A. Papadopoulos, W. C. Wester, Robert Connon Smith, Manda Banerji, Flavia Sobreira, Gary Bernstein, Jon J Thaler, Alex Merson, G. Gutierrez, P. Guarnieri, Brian Nord, G. B. Caminha, Basilio X. Santiago, Joseph J. Mohr, Eduardo Balbinot, S. L. Reed, Ricardo L. C. Ogando, Juan Estrada, Adam Amara, Risa H. Wechsler, E. Suchyta, August E. Evrard, Joaquin Vieira, Alexandre Refregier, Robert J. Brunner, Krishna Naidoo, Tianjun Li, Joshua A. Frieman, A. Roodman, Tommaso Giannantonio, I. Sevilla-Noarbe, Christopher J. Conselice, Claudia Maraston, A. A. Plazas, Diego Capozzi, L. N. da Costa, Robert C. Nichol, J. Carretero, D. W. Gerdes, Tamara M. Davis, Peter Melchior, Enrique Gaztanaga, Daniel A. Goldstein, Marc Manera, Francisco J. Castander, J. P. Dietrich, Richard G. McMahon, J. Carlsen, D. A. Finley, Mark Sullivan, Juan Garcia-Bellido, Eduardo Rozo, Jelena Aleksić, R. C. Thomas, Eli S. Rykoff, Richard G. Kron, K. Honscheid, Marcos Lima, Douglas L. Tucker, Kyler Kuehn, Jonathan Blazek, Sarah Bridle, Scott Dodelson, Carlos E. Cunha, Martin Makler, M. Sako, Richard Kessler, and G. Tarle
- Subjects
Cosmology and Gravitation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,supernovae ,astro-ph.GA ,quasars ,FOS: Physical sciences ,Library science ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Galaxies general ,surveys ,minor plantes, asteroids ,galaxies ,0103 physical sciences ,media_common.cataloged_instance ,Deslocamento para o vermelho ,European union ,Astronomy observatory ,Galáxias ,010303 astronomy & astrophysics ,STFC ,Astrophysics::Galaxy Astrophysics ,media_common ,QB ,Physics ,Mapeamentos astronômicos ,010308 nuclear & particles physics ,Surveys minor planets ,European research ,RCUK ,Astronomy ,Astronomy and Astrophysics ,Asteroids general ,Astrophysics - Astrophysics of Galaxies ,Quasars general ,Supernovae general ,Galaxy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Fundamental physics ,astro-ph.CO ,Christian ministry ,Galaxy general ,National laboratory ,surveys – minor planets, asteroids: general – supernovae: general – Galaxy: general – galaxies: general – quasars: general ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
This overview article describes the legacy prospect and discovery potential of the Dark Energy Survey (DES) beyond cosmological studies, illustrating it with examples from the DES early data. DES is using a wide-field camera (DECam) on the 4m Blanco Telescope in Chile to image 5000 sq deg of the sky in five filters (grizY). By its completion the survey is expected to have generated a catalogue of 300 million galaxies with photometric redshifts and 100 million stars. In addition, a time-domain survey search over 27 sq deg is expected to yield a sample of thousands of Type Ia supernovae and other transients. The main goals of DES are to characterise dark energy and dark matter, and to test alternative models of gravity; these goals will be pursued by studying large scale structure, cluster counts, weak gravitational lensing and Type Ia supernovae. However, DES also provides a rich data set which allows us to study many other aspects of astrophysics. In this paper we focus on additional science with DES, emphasizing areas where the survey makes a difference with respect to other current surveys. The paper illustrates, using early data (from `Science Verification', and from the first, second and third seasons of observations), what DES can tell us about the solar system, the Milky Way, galaxy evolution, quasars, and other topics. In addition, we show that if the cosmological model is assumed to be Lambda+ Cold Dark Matter (LCDM) then important astrophysics can be deduced from the primary DES probes. Highlights from DES early data include the discovery of 34 Trans Neptunian Objects, 17 dwarf satellites of the Milky Way, one published z > 6 quasar (and more confirmed) and two published superluminous supernovae (and more confirmed)., 32 pages, 15 figures; a revised Figure 1 and minor changes, to match the published MNRAS version
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- 2016
39. A DECAM SEARCH FOR AN OPTICAL COUNTERPART TO THE LIGO GRAVITATIONAL-WAVE EVENT GW151226
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Wen-fai Fong, Brian Yanny, Shantanu Desai, John Marriner, A. K. Romer, D. L. Burke, R. C. Thomas, A. A. Plazas, A. Fausti Neto, Armin Rest, A. Carnero Rosell, D. L. Tucker, Eliot Quataert, Richard Kessler, William Wester, Kyler Kuehn, V. A. Villar, E. Suchyta, August E. Evrard, Philip S. Cowperthwaite, A. Benoit-Lévy, Keith Bechtol, K. Honscheid, Kevin Reil, M. Carrasco Kind, Robert C. Nichol, Peter K. G. Williams, Daniel Scolnic, G. Strampelli, Eric H. Neilsen, Marcos Lima, D. J. Brout, V. Scarpine, Felipe Menanteau, Edo Berger, Alex Drlica-Wagner, Derek B. Fox, Brian Nord, Gregory Tarle, Daniel Kasen, Raffaella Margutti, G. Gutierrez, Masao Sako, R. C. Smith, Carlos Cunha, I. Sevilla-Noarbe, Huan Lin, Juan Garcia-Bellido, Ryan Chornock, Ben Farr, David J. James, Ramon Miquel, Brian D. Metzger, Pablo Fosalba, Robert Armstrong, L. N. da Costa, Duncan A. Brown, Alistair R. Walker, S. Allam, Robert A. Gruendl, Hsin-Yu Chen, Maria R. Drout, Marcelle Soares-Santos, J. Annis, Zoheyr Doctor, Flavia Sobreira, Thomas Matheson, M. W. G. Johnson, Jennifer L. Marshall, S. B. Cenko, F. B. Abdalla, Elisabeth Krause, Joseph J. Mohr, Joshua A. Frieman, Tommaso Giannantonio, H. T. Diehl, M. S. S. Gill, Daniel Thomas, E. Buckley-Geer, David Brooks, Francisco J. Castander, E. Bertin, Marcio A. G. Maia, Michael D. Johnson, Ken Herner, Nathan Smith, Daniel Gruen, D. A. Finley, J. Carretero, D. W. Gerdes, Daniel A. Goldstein, J. P. Dietrich, Jochen Weller, T. M. C. Abbott, R. J. Foley, E. J. Sanchez, C. B. D'Andrea, Nikolay Kuropatkin, Daniel E. Holz, Ricardo L. C. Ogando, UAM. Departamento de Física Teórica, Harvard Smithsonian Ctr Astrophys, Fermilab Natl Accelerator Lab, Univ Penn, Syracuse Univ, NASA, Univ Maryland, Univ Chicago, Ohio Univ, Univ Calif Santa Cruz, Univ Illinois, Univ Arizona, Penn State Univ, Univ Autonoma Madrid, Stanford Univ, SLAC Natl Accelerator Lab, Natl Ctr Supercomputing Applicat, Univ Calif Berkeley, Lawrence Berkeley Natl Lab, NYU, Natl Opt Astron Observ, Columbia Univ, Space Telescope Sci Inst, Universidade Estadual Paulista (Unesp), Lab Interinst E Astron LIneA, UCL, Rhodes Univ, Princeton Univ, Univ Wisconsin, CNRS, Univ Paris 06, Observ Nacl, IEEC CSIC, Barcelona Inst Sci & Technol, Univ Portsmouth, Univ Southampton, Univ Munich, Excellence Cluster Universe, Univ Michigan, Univ Cambridge, Ohio State Univ, Australian Astron Observ, Universidade de São Paulo (USP), Texas A&M Univ, Inst Catalana Recerca & Estudis Avancats, Max Planck Inst Extraterr Phys, CALTECH, Univ Sussex, and Ctr Invest Energet Medioambientales & Tecnol CIEM
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,close [binaries] ,FOS: Physical sciences ,Astrophysics ,Surveys ,Kilonova ,Astronomy & Astrophysics ,01 natural sciences ,Gravitational waves ,neutron [stars] ,surveys ,Stars: Neutron ,0103 physical sciences ,GW151226 ,010303 astronomy & astrophysics ,STFC ,QB ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,astro-ph.HE ,010308 nuclear & particles physics ,Gravitational wave ,Detector ,Física ,RCUK ,Astronomy and Astrophysics ,Galaxy ,LIGO ,Binaries: Close ,Supernova ,gravitational waves ,13. Climate action ,Space and Planetary Science ,Dark energy ,astro-ph.CO ,Catalogs ,Astrophysics - High Energy Astrophysical Phenomena ,catalogs ,Astronomical and Space Sciences ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Astrophysical Journal Letters 826.2 (2016): L29 reproduced by permission of the AAS, We report the results of a Dark Energy Camera optical follow-up of the gravitational-wave (GW) event GW151226, discovered by the Advanced Laser Interferometer Gravitational-wave Observatory detectors. Our observations cover 28.8 deg2 of the localization region in the i and z bands (containing 3% of the BAYESTAR localization probability), starting 10 hr after the event was announced and spanning four epochs at 2-24 days after the GW detection. We achieve 5σ point-source limiting magnitudes of i ≈ 21.7 and z ≈ 21.5, with a scatter of 0.4 mag, in our difference images. Given the two-day delay, we search this area for a rapidly declining optical counterpart with ≥ 3σ significance steady decline between the first and final observations. We recover four sources that pass our selection criteria, of which three are cataloged active galactic nuclei. The fourth source is offset by 5.8 arcsec from the center of a galaxy at a distance of 187 Mpc, exhibits a rapid decline by 0.5 mag over 4 days, and has a red color of i - z ≈ 0.3 mag. These properties could satisfy a set of cuts designed to identify kilonovae. However, this source was detected several times, starting 94 days prior to GW151226, in the Pan-STARRS Survey for Transients (dubbed as PS15cdi) and is therefore unrelated to the GW event. Given its long-term behavior, PS15cdi is likely a Type IIP supernova that transitioned out of its plateau phase during our observations, mimicking a kilonova-like behavior. We comment on the implications of this detection for contamination in future optical follow-up observations, P.S.C. is grateful for support provided by the NSF through the Graduate Research Fellowship Program, grant DGE1144152. R. J.F. gratefully acknowledges support from NSF grant AST– 1518052 and the Alfred P. Sloan Foundation. D.E.H. was supported by NSF CAREER grant PHY-1151836. He also acknowledges support from the Kavli Institute for Cosmological Physics at the University of Chicago through NSF grant PHY- 1125897 as well as an endowment from the Kavli Foundation. The DES Data Management System is supported by the NSF under grant number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the ERC under the EU’s 7th Framework Programme including grants ERC 240672, 291329,and 306478
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- 2016
40. Cosmic shear measurements with Dark Energy Survey Science Verification data
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A. Roodman, A. K. Romer, Darren L. DePoy, A. Fausti Neto, M. Sako, Marcos Lima, Andrina Nicola, D. L. Burke, J. Carretero, T. Kacprzak, E. Suchyta, August E. Evrard, Andrey V. Kravtsov, Francisco J. Castander, G. Gutierrez, Alexandre Refregier, Matthew R. Becker, Flavia Sobreira, Cristiano G. Sabiu, S. Allam, Robert A. Gruendl, Joseph J. Mohr, J. P. Dietrich, A. A. Plazas, Gary Bernstein, Vinu Vikram, Diego Capozzi, A. Benoit-Lévy, M. T. Busha, David Brooks, M. E. C. Swanson, M. Carrasco Kind, Ofer Lahav, Eli S. Rykoff, David J. James, Michael Schubnell, Robert C. Nichol, William G. Hartley, Risa H. Wechsler, Matt J. Jarvis, Peter Doel, T. M. C. Abbott, Tim Eifler, Pablo Fosalba, V. Scarpine, Kevin Reil, Hiranya V. Peiris, Carles Sanchez, M. March, Enrique Gaztanaga, Oliver Friedrich, H. T. Diehl, Peter Melchior, E. J. Sanchez, R. C. Smith, David Bacon, Joe Zuntz, Daniel Gruen, Boris Leistedt, Robert Armstrong, A. H. Bauer, Niall MacCrann, B. Flaugher, C. B. D'Andrea, E. Sheldon, Brandon M. S. Erickson, E. Bertin, Ramon Miquel, Daniel Thomas, E. Buckley-Geer, Martin Crocce, Adam Amara, A. Carnero Rosell, C. Bonnett, Shantanu Desai, D. A. Finley, P. Martini, D. W. Gerdes, Bhuvnesh Jain, J. J. Thaler, Sarah Bridle, Scott Dodelson, Elisabeth Krause, Chihway Chang, Carlos E. Cunha, F. B. Abdalla, Donnacha Kirk, E. Fernandez, Alistair R. Walker, K. Honscheid, Marcelle Soares-Santos, C. J. Miller, Hee-Jong Seo, Ricardo L. C. Ogando, Brian Nord, Gregory Tarle, M. A. G. Maia, I. Sevilla-Noarbe, N. Kuropatkin, L. N. da Costa, M. Banerji, Joshua A. Frieman, Kyler Kuehn, Michael Troxel, and Tianjun Li
- Subjects
IMPACT ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Astronomy & Astrophysics ,01 natural sciences ,Physics, Particles & Fields ,0103 physical sciences ,Sample variance ,Statistical physics ,COVARIANCE ,NOISE BIAS ,010303 astronomy & astrophysics ,Weak gravitational lensing ,QB ,Physics ,Science & Technology ,COSMIC cancer database ,010308 nuclear & particles physics ,Covariance matrix ,WEAK LENSING SURVEYS ,GALAXY SHAPE MEASUREMENT ,STATISTICS ,SIMULATIONS ,Galaxy ,POLARIZATION POWER SPECTRA ,MODEL ,Physical Sciences ,astro-ph.CO ,Dark energy ,Halo ,MATTER ,Jackknife resampling - Abstract
We present measurements of weak gravitational lensing cosmic shear two-point statistics using Dark Energy Survey Science Verification data. We demonstrate that our results are robust to the choice of shear measurement pipeline, either ngmix or im3shape, and robust to the choice of two-point statistic, including both real and Fourier-space statistics. Our results pass a suite of null tests including tests for B-mode contamination and direct tests for any dependence of the two-point functions on a set of 16 observing conditions and galaxy properties, such as seeing, airmass, galaxy color, galaxy magnitude, etc. We furthermore use a large suite of simulations to compute the covariance matrix of the cosmic shear measurements and assign statistical significance to our null tests. We find that our covariance matrix is consistent with the halo model prediction, indicating that it has the appropriate level of halo sample variance. We compare the same jackknife procedure applied to the data and the simulations in order to search for additional sources of noise not captured by the simulations. We find no statistically significant extra sources of noise in the data. The overall detection significance with tomography for our highest source density catalog is 9.7 sigma . Cosmological constraints from the measurements in this work are presented in a companion paper [DES et al., Phys. Rev. D 94, 022001 (2016).].
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- 2016
41. Cosmology constraints from shear peak statistics in Dark Energy Survey Science Verification data
- Author
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Laura Marian, Ofer Lahav, Joe Zuntz, Eli S. Rykoff, Tim Eifler, Gregory Tarle, A. Carnero Rosell, J. Carretero, R. C. Smith, Daniel A. Goldstein, K. Honscheid, V. Scarpine, B. Flaugher, Shantanu Desai, H. T. Diehl, Bhuvnesh Jain, J. P. Dietrich, David Bacon, E. Sheldon, W. G. Hartley, Sarah Bridle, Niall MacCrann, Jennifer L. Marshall, Nikolay Kuropatkin, Chihway Chang, Martin Crocce, M. Carrasco Kind, Peter Melchior, Yanming Zhang, D. L. Burke, Kyler Kuehn, Josh Frieman, Adam Amara, Robert C. Nichol, Gary Bernstein, F. B. Abdalla, Brian Nord, Matthew R. Becker, Flavia Sobreira, Jochen Weller, P. Martini, David Brooks, David J. James, M. E. C. Swanson, A. Roodman, G. Gutierrez, E. Bertin, S. Samuroff, Pablo Fosalba, V. Vikram, T. M. C. Abbott, A. A. Plazas, A. K. Romer, J. Aleksić, M. March, Robert A. Gruendl, Donnacha Kirk, E. J. Sanchez, Michael Troxel, Alistair R. Walker, A. Benoit-Lévy, A. Fausti Neto, M. Jarvis, Marcelle Soares-Santos, Ramon Miquel, C. B. D'Andrea, Daniel Thomas, T. Kacprzak, Elisabeth Krause, I. Sevilla-Noarbe, E. M. Huff, L. N. da Costa, Oliver Friedrich, Michael Schubnell, Joseph J. Mohr, Robert Armstrong, E. Suchyta, August E. Evrard, C. Bonnett, Alexandre Refregier, Andrina Nicola, Marcos Lima, R. A. Bernstein, C. J. Miller, Daniel Gruen, D. W. Gerdes, and Francisco J. Castander
- Subjects
Cosmology and Gravitation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,statistical [methods] ,Dark matter ,Gravitational lensing formalism ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,dark matter ,Cosmology ,Methods statistical ,weak [gravitational lensing] ,0103 physical sciences ,Statistics ,data analysis [methods] ,010303 astronomy & astrophysics ,STFC ,Weak gravitational lensing ,QB ,Physics ,010308 nuclear & particles physics ,RCUK ,Astronomy and Astrophysics ,observations [cosmology] ,Shear (geology) ,Space and Planetary Science ,astro-ph.CO ,Dark energy ,cosmological parameter ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Shear peak statistics has gained a lot of attention recently as a practical alternative to the two point statistics for constraining cosmological parameters. We perform a shear peak statistics analysis of the Dark Energy Survey (DES) Science Verification (SV) data, using weak gravitational lensing measurements from a 139 deg$^2$ field. We measure the abundance of peaks identified in aperture mass maps, as a function of their signal-to-noise ratio, in the signal-to-noise range $04$ would require significant corrections, which is why we do not include them in our analysis. We compare our results to the cosmological constraints from the two point analysis on the SV field and find them to be in good agreement in both the central value and its uncertainty. We discuss prospects for future peak statistics analysis with upcoming DES data., Comment: 21 pages, 14 figures, submitted to MNRAS
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- 2016
42. CMB lensing tomography with the DES Science Verification galaxies
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Flavia Sobreira, Ricardo L. C. Ogando, Peter Doel, Martin Crocce, H. T. Diehl, Jennifer L. Marshall, T. M. Crawford, Robert Crittenden, Robert Connon Smith, W. L. Holzapfel, A. H. Bauer, G. Simard, E. Fernandez, M. March, M. Carrasco Kind, I. Sevilla-Noarbe, E. Suchyta, August E. Evrard, L. N. da Costa, Robert C. Nichol, Peter Melchior, F. B. Abdalla, E. Bertin, K. T. Story, B. Soergel, C. L. Chang, Benjamin Saliwanchik, Gary Bernstein, A. Benoit-Lévy, J. Carretero, Brian Nord, M. Sako, Joshua A. Frieman, A. Roodman, Manda Banerji, Tommaso Giannantonio, Dragan Huterer, Vinu Vikram, G. Gutierrez, J. P. Dietrich, Enrique Gaztanaga, Bradford Benson, Robert Armstrong, B. Flaugher, Kyler Kuehn, D. L. Burke, Nikolay Kuropatkin, S. Allam, Robert A. Gruendl, D. A. Finley, Elisabeth Krause, A. K. Romer, Paul Martini, A. Fausti Neto, Tim Eifler, Jochen Weller, Marcos Lima, Ramon Miquel, Will J. Percival, T. M. C. Abbott, Antony A. Stark, Risa H. Wechsler, Joaquin Vieira, Gregory Tarle, Hiranya V. Peiris, Tianjun Li, Eli S. Rykoff, Ofer Lahav, E. J. Sanchez, A. Carnero Rosell, K. Honscheid, Scott Dodelson, Y. Omori, Carlos E. Cunha, Bhuvnesh Jain, R. A. Bernstein, Joe Zuntz, David J. James, Pablo Fosalba, Shantanu Desai, David Brooks, M. E. C. Swanson, Darren L. DePoy, Ashley J. Ross, John E. Carlstrom, J. J. Thaler, A. A. Plazas, Diego Capozzi, Joseph J. Mohr, C. B. D'Andrea, Donnacha Kirk, Alistair R. Walker, Michael Schubnell, Christian L. Reichardt, Marcelle Soares-Santos, R. Cawthon, Daniel Thomas, E. Buckley-Geer, F. Elsner, Gilbert Holder, Francisco J. Castander, Daniel Gruen, D. W. Gerdes, and Boris Leistedt
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Cosmology and Gravitation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,ANGULAR POWER SPECTRUM ,Cosmic microwave background ,Dark matter ,STOCHASTIC BIAS ,FOS: Physical sciences ,cosmic background radiation ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,01 natural sciences ,INTEGRATED SACHS-WOLFE ,gravitational lensing: weak ,weak [gravitational lensing] ,Observational cosmology ,LARGE-SCALE STRUCTURE ,0201 Astronomical and Space Sciences ,0103 physical sciences ,100 SQUARE DEGREES ,010303 astronomy & astrophysics ,STFC ,Weak gravitational lensing ,Astrophysics::Galaxy Astrophysics ,QB ,Physics ,Science & Technology ,DARK ENERGY SURVEY ,010308 nuclear & particles physics ,RCUK ,Astronomy ,Astronomy and Astrophysics ,Redshift survey ,ST/L000636/1 ,Redshift ,CHALLENGE LIGHTCONE SIMULATION ,South Pole Telescope ,MICROWAVE BACKGROUND ANISOTROPIES ,Space and Planetary Science ,Physical Sciences ,CROSS-CORRELATION ,astro-ph.CO ,Dark energy ,large-scale structure of Universe ,ATACAMA COSMOLOGY TELESCOPE ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We measure the cross-correlation between the galaxy density in the Dark Energy Survey (DES) Science Verification data and the lensing of the cosmic microwave background (CMB) as reconstructed with the Planck satellite and the South Pole Telescope (SPT). When using the DES main galaxy sample over the full redshift range $0.2 < z < 1.2$, a cross-correlation signal is detected at $6 \sigma$ and $4\sigma$ with SPT and Planck respectively. We then divide the DES galaxies into five photometric redshift bins, finding significant ($>$$2 \sigma$) detections in all bins. Comparing to the fiducial Planck cosmology, we find the redshift evolution of the signal matches expectations, although the amplitude is consistently lower than predicted across redshift bins. We test for possible systematics that could affect our result and find no evidence for significant contamination. Finally, we demonstrate how these measurements can be used to constrain the growth of structure across cosmic time. We find the data are fit by a model in which the amplitude of structure in the $z, Comment: 32 pages, 29 figures, minor modifications to match version published by MNRAS
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- 2016
43. THE ALHAMBRA SURVEY: EVOLUTION OF GALAXY SPECTRAL SEGREGATION
- Author
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Mirjana Pović, Francisco J. Castander, Tom Broadhurst, Narciso Benítez, Emilio J. Alfaro, T. Aparicio-Villegas, A. del Olmo, Leopoldo Infante, David Cristóbal-Hornillos, J. Cepa, Pablo Arnalte-Mur, J. A. L. Aguerri, Ll. Hurtado-Gil, Silvestre Paredes, C. Husillos, Francisco Prada, Jesús Cabrera-Caño, Jaime Perea, Vicent J. Martínez, R. M. González Delgado, C. López-Sanjuan, Alberto Molino, Kerttu Viironen, Miguel Cerviño, Mariano Moles, I. Márquez, J. Masegosa, B. Ascaso, Mauro Stefanon, Alberto Fernández-Soto, J. M. Quintana, Department of Chemistry and Institute for Nanoscale Physics and chemistry (INPAC), Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Spanish National Research Council (CSIC), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), AUTRES, Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 'Federico II' University of Naples Medical School, Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universidad de Sevilla. Departamento de Física Atómica, Molecular y Nuclear, Ministerio de Economía y Competitividad (MINECO). España, Junta de Andalucía, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidad Autónoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), European Commission, Ministerio de Economía y Competitividad (España), Generalitat Valenciana, Generalitat de Catalunya, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), and UAM. Departamento de Física Teórica
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statistical [Methods] ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Large-scale structure of universe ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Methods statistical ,Galaxies: distances and redshifts ,Methods: data analysis ,0103 physical sciences ,distances and redshifts [Galaxies] ,observations [Cosmology] ,data analysis [Methods] ,010303 astronomy & astrophysics ,Methods: statistical ,Astrophysics::Galaxy Astrophysics ,ComputingMilieux_MISCELLANEOUS ,Physics ,[PHYS]Physics [physics] ,010308 nuclear & particles physics ,Cosmology: observations ,Física ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
arXiv:1601.03668v1, We study the clustering of galaxies as a function of spectral type and redshift in the range 0.35, This work was mainly supported by the Spanish Ministry for Economy and Competitiveness and FEDER funds through grants AYA2010-22111-C03-02 and AYA2013-48623-C2-2, and by the Generalitat Valenciana through project PrometeoII 2014/060. We also acknowledge support from the Spanish Ministry for Economy and Competitiveness and FEDER funds through grants AYA2012-39620, AYA2013-40611-P, AYA2013-42227-P, AYA2013-43188-P, AYA2013-48623-C2-1, ESP2013-48274, AYA2014-58861-C3-1, Junta de Andalucia grants TIC114, JA2828, P10-FQM-6444, and Generalitat de Catalunya project SGR-1398. Begona Ascaso acknowledge funding from the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 656354.
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- 2016
44. Galaxy clustering, photometric redshifts and diagnosis of systematics in the DES Science Verification data
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Tommaso Giannantonio, Gregory Tarle, Tim Eifler, J. J. Thaler, B. Flaugher, Kyler Kuehn, Ricardo L. C. Ogando, Ofer Lahav, Robert J. Brunner, Carlos E. Cunha, Robert Connon Smith, K. Honscheid, R. Cawthon, G. Gutierrez, Boris Leistedt, Eric H. Neilsen, Nikolay Kuropatkin, J. Carretero, David J. James, Martin Crocce, Jochen Weller, M. Carrasco Kind, Eli S. Rykoff, M. Sako, H. T. Diehl, Robert C. Nichol, Pablo Fosalba, Brian Nord, T. M. C. Abbott, Hiranya V. Peiris, Daniel Thomas, David Brooks, M. E. C. Swanson, A. A. Plazas, M. A. G. Maia, E. J. Sanchez, A. Carnero Rosell, A. H. Bauer, E. Fernandez, Francisco J. Castander, E. Buckley-Geer, Diego Capozzi, E. Suchyta, Risa H. Wechsler, D. L. Burke, Michael Schubnell, Marcos Lima, August E. Evrard, Joe Zuntz, Edward J. Kim, Jennifer L. Marshall, Ashley J. Ross, Alistair R. Walker, C. B. D'Andrea, Tianjun Li, A. Benoit-Lévy, S. Allam, Robert A. Gruendl, Marcelle Soares-Santos, C. Bonnett, Ramon Miquel, Carles Sanchez, Shantanu Desai, Enrique Gaztanaga, F. B. Abdalla, E. Bertin, Will J. Percival, A. K. Romer, Gary Bernstein, Paul Martini, Javier Sanchez, Daniel Gruen, William G. Hartley, A. Fausti Neto, Peter Melchior, D. A. Finley, Vinu Vikram, Rogerio Rosenfeld, D. W. Gerdes, C. J. Miller, Flavia Sobreira, M. March, Basilio X. Santiago, I. Sevilla-Noarbe, L. N. da Costa, M. Banerji, Joshua A. Frieman, IEEC CSIC, Univ Autonoma Barcelona, Ohio State Univ, Ctr Invest Energet Medioambientales & Tecnol CIEM, Univ Illinois, Univ Cambridge, Fermilab Natl Accelerator Lab, Lab Interinst & E Astron LIneA, UCL, Observ Nacl, Univ Chicago, ETH, Univ Portsmouth, Universidade Estadual Paulista (Unesp), Stanford Univ, SLAC Natl Accelerator Lab, Cerro Tololo Interamer Observ, Rhodes Univ, Univ Calif Berkeley, Univ Penn, CNRS, Univ Paris 06, Excellence Cluster Universe, Univ Munich, CALTECH, Univ Michigan, Max Planck Inst Extraterr Phys, Australian Astron Observ, Texas A&M Univ, Universidade de São Paulo (USP), Univ Sussex, Univ Fed Rio Grande do Sul, Argonne Natl Lab, and Univ Manchester
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systematic effects ,Cosmology and Gravitation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cold dark matter ,Dark matter ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Surveys ,01 natural sciences ,symbols.namesake ,0103 physical sciences ,surveys - cosmology ,observations - large-scale structure of Universe ,Planck ,Galáxias ,observations [Cosmology] ,Cluster analysis ,010303 astronomy & astrophysics ,STFC ,Astrophysics::Galaxy Astrophysics ,Photometric redshift ,QB ,Mapeamentos astronômicos ,Physics ,010308 nuclear & particles physics ,photometric surveys ,RCUK ,Astronomy ,Astronomy and Astrophysics ,galaxies clustering ,Galaxy ,Redshift ,13. Climate action ,Space and Planetary Science ,astro-ph.CO ,Dark energy ,symbols ,large-scale structure of Universe ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We study the clustering of galaxies detected at $i, Comment: 23 pages, 18 figures, matches the version published in MNRAS. MNRAS 455, 4301-4324 (2015)
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- 2016
45. The DES Science Verification weak lensing shear catalogues
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Daniel Thomas, E. Buckley-Geer, T. Kacprzak, Michael Schubnell, Brian Nord, Eli S. Rykoff, I. Sevilla-Noarbe, Tim Eifler, B. Flaugher, Ricardo L. C. Ogando, M. Jarvis, C. B. D'Andrea, E. Sheldon, G. Gutierrez, Peter Melchior, Nikolay Kuropatkin, Darren L. DePoy, L. N. da Costa, S. Samuroff, A. Carnero Rosell, Peter Doel, David Brooks, M. E. C. Swanson, Joseph Clampitt, Marcos Lima, Barnaby Rowe, A. K. Romer, Alex Drlica-Wagner, Donnacha Kirk, David J. James, Joseph J. Mohr, Alistair R. Walker, K. Honscheid, Matthew R. Becker, Flavia Sobreira, H. T. Diehl, Michael Troxel, J. J. Thaler, A. Fausti Neto, Francisco J. Castander, E. M. Huff, Marcelle Soares-Santos, Joshua A. Frieman, Michael Hirsch, Pablo Fosalba, M. Carrasco Kind, J. Carretero, Kyler Kuehn, D. L. Burke, M. March, R. C. Smith, Niall MacCrann, J. P. Dietrich, Gregory Tarle, Robert Armstrong, M. Sako, Adam Amara, Kevin Reil, S. Allam, Robert A. Gruendl, E. Suchyta, J. Annis, C. Bonnett, Carles Sanchez, Alexandre Refregier, Enrique Gaztanaga, Shantanu Desai, Daniel Gruen, D. W. Gerdes, C. Gangkofner, Steve Kent, F. B. Abdalla, E. Bertin, A. A. Plazas, Diego Capozzi, Gary Bernstein, Bhuvnesh Jain, Vinu Vikram, V. Scarpine, Ofer Lahav, Eric H. Neilsen, Martin Crocce, P. Martini, Joe Zuntz, A. Benoit-Lévy, Risa H. Wechsler, Tianjun Li, A. Roodman, R. Das, Ramon Miquel, T. M. C. Abbott, E. J. Sanchez, Sarah Bridle, Chihway Chang, and Carlos E. Cunha
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Point spread function ,Systematic error ,Cosmology and Gravitation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,FOS: Physical sciences ,Astrophysics ,Surveys ,01 natural sciences ,0103 physical sciences ,image processing [Techniques] ,observations [Cosmology] ,data analysis [Methods] ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,STFC ,Weak gravitational lensing ,QB ,Physics ,010308 nuclear & particles physics ,RCUK ,Astronomy and Astrophysics ,Geodesy ,Catalogues ,Galaxy ,Shear (geology) ,Space and Planetary Science ,astro-ph.CO ,Dark energy ,Astrophysics - Instrumentation and Methods for Astrophysics ,weak [Gravitational lensing] ,astro-ph.IM ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present weak lensing shear catalogues for 139 square degrees of data taken during the Science Verification (SV) time for the new Dark Energy Camera (DECam) being used for the Dark Energy Survey (DES). We describe our object selection, point spread function estimation and shear measurement procedures using two independent shear pipelines, IM3SHAPE and NGMIX, which produce catalogues of 2.12 million and 3.44 million galaxies respectively. We detail a set of null tests for the shear measurements and find that they pass the requirements for systematic errors at the level necessary for weak lensing science applications using the SV data. We also discuss some of the planned algorithmic improvements that will be necessary to produce sufficiently accurate shear catalogues for the full 5-year DES, which is expected to cover 5000 square degrees., Accepted by MNRAS; 38 pages, 29 figures; v3: minor edits based on referee's comments, switched to mnras style, added figure 8, updated info about released catalogs
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- 2016
46. Detection of the kinematic Sunyaev-Zel'dovich effect with DES Year 1 and SPT
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T. de Haan, Eli S. Rykoff, K. T. Story, Ramon Miquel, Ryan Keisler, Bradford Benson, Salman Habib, M. Carrasco Kind, Robert Armstrong, J. P. Dietrich, Nathan Whitehorn, I-Non Chiu, A. Carnero Rosell, Eduardo Rozo, Martin Crocce, Alistair R. Walker, John E. Carlstrom, I. Sevilla-Noarbe, Ricardo L. C. Ogando, Marcelle Soares-Santos, Michael McDonald, B. Soergel, N. Kuropatkin, Scott Dodelson, Kyler Kuehn, Jennifer L. Marshall, Carlos E. Cunha, L. N. da Costa, T. M. Crawford, A. Roodman, Tommaso Giannantonio, Shantanu Desai, W. L. Holzapfel, B. Flaugher, R. Chown, E. Suchyta, Peter Doel, A. Saro, August E. Evrard, Peter Melchior, Katrin Heitmann, F. B. Abdalla, Gregory Tarle, A. K. Romer, C. B. D'Andrea, H. T. Diehl, Juan Estrada, Samuel Flender, K. Honscheid, A. A. Plazas, Daniel Thomas, Gary Bernstein, Lindsey Bleem, Ofer Lahav, Antony A. Stark, David Rapetti, Erin Sheldon, M. E. C. Swanson, Robert Connon Smith, Jochen Weller, Enrique Gaztanaga, Joaquin Vieira, Michael Schubnell, David J. James, Daniel Gruen, Brian Nord, E. J. Sanchez, Christian L. Reichardt, Joshua A. Frieman, Pablo Fosalba, S. Allam, Robert A. Gruendl, George Efstathiou, Y. Omori, Francisco J. Castander, Bhuvnesh Jain, Benjamin Saliwanchik, Gilbert Holder, A. Benoit-Lévy, C. J. Miller, Marcos Lima, J. Annis, Flavia Sobreira, Soergel, B., Flender, S., Story, K. T., Bleem, L., Giannantonio, T., Efstathiou, G., Rykoff, E., Benson, B. A., Crawford, T., Dodelson, S., Habib, S., Heitmann, K., Holder, G., Jain, B., Rozo, E., Saro, A., Weller, J., Abdalla, F. B., Allam, S., Annis, J., Armstrong, R., Benoit-Ĺevy, A., Bernstein, G. M., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Chiu, I., Chown, R., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., de Haan, T., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Estrada, J., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Holzapfel, W. L., Honscheid, K., James, D. J., Keisler, R., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Marshall, J. L., Mcdonald, M., Melchior, P., Miller, C. J., Miquel, R., Nord, B., Ogando, R., Omori, Y., Plazas, A. A., Rapetti, D., Reichardt, C. L., Romer, A. K., Roodman, A., Saliwanchik, B. R., Sanchez, E., Schubnell, M., Sevilla-Noarbe, I., Sheldon, E., Smith, R. C., Soares-Santos, M., Sobreira, F., Stark, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vieira, J. D., Walker, A. R., and Whitehorn, N.
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Cosmology and Gravitation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Large-scale structure of Universe ,Library science ,FOS: Physical sciences ,cosmic background radiation ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Cosmic background radiation ,01 natural sciences ,0103 physical sciences ,media_common.cataloged_instance ,clusters: general [galaxies] ,European union ,Astronomy observatory ,010303 astronomy & astrophysics ,STFC ,media_common ,QB ,Physics ,010308 nuclear & particles physics ,European research ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,RCUK ,Astronomy and Astrophysics ,Astronomy and Astrophysic ,ST/L000636/1 ,Research council ,Space and Planetary Science ,Galaxies: clusters: general ,Fundamental physics ,astro-ph.CO ,Christian ministry ,large-scale structure of Universe ,National laboratory ,Data release ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We detect the kinematic Sunyaev-Zel'dovich (kSZ) effect with a statistical significance of $4.2 \sigma$ by combining a cluster catalogue derived from the first year data of the Dark Energy Survey (DES) with CMB temperature maps from the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) Survey. This measurement is performed with a differential statistic that isolates the pairwise kSZ signal, providing the first detection of the large-scale, pairwise motion of clusters using redshifts derived from photometric data. By fitting the pairwise kSZ signal to a theoretical template we measure the average central optical depth of the cluster sample, $\bar{\tau}_e = (3.75 \pm 0.89)\cdot 10^{-3}$. We compare the extracted signal to realistic simulations and find good agreement with respect to the signal-to-noise, the constraint on $\bar{\tau}_e$, and the corresponding gas fraction. High-precision measurements of the pairwise kSZ signal with future data will be able to place constraints on the baryonic physics of galaxy clusters, and could be used to probe gravity on scales $ \gtrsim 100$ Mpc., Comment: 23 pages, 14 figures; matches version published in MNRAS
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- 2016
- Full Text
- View/download PDF
47. THE REDMAPPER GALAXY CLUSTER CATALOG from des SCIENCE VERIFICATION DATA
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N. Kuropatkin, Daniel Gruen, M. Carrasco Kind, Brian Nord, Geraint F. Lewis, Flavia Sobreira, Robert C. Nichol, Eduardo Rozo, Michael Schubnell, Ramon Miquel, John P. Stott, G. Gutierrez, E. Bertin, Basilio X. Santiago, E. Suchyta, Risa H. Wechsler, M. Childress, A. K. Romer, D. A. Finley, Robert G. Mann, Syed Uddin, Ricardo L. C. Ogando, August E. Evrard, Shantanu Desai, A. Benoit-Lévy, Ben Hoyle, Gary Bernstein, David Brooks, M. E. C. Swanson, Paul Martini, Matt Hilton, C. Vergara Cervantes, Marcos Lima, Douglas L. Tucker, Jennifer L. Marshall, Tamara M. Davis, Daniel A. Goldstein, A. Saro, Kyler Kuehn, J. P. Dietrich, I. Sevilla-Noarbe, F. B. Abdalla, J. Annis, Joseph J. Mohr, Gregory Tarle, Eli S. Rykoff, Peter Melchior, Ofer Lahav, Francisco J. Castander, Peter Doel, A. A. Plazas, H. T. Diehl, Yanming Zhang, A. Carnero Rosell, Julian A. Mayers, C. Lidman, A. Bermeo-Hernandez, David J. James, Carlos E. Cunha, Diego Capozzi, Alistair R. Walker, Pablo Fosalba, Marcelle Soares-Santos, K. Honscheid, Karl Glazebrook, V. Vikram, L. N. da Costa, H. Wilcox, Christopher J. Miller, Kevin Reil, Tesla E. Jeltema, Pedro T. P. Viana, R. C. Smith, T. M. C. Abbott, Daniel Thomas, V. Scarpine, Joshua A. Frieman, E. J. Sanchez, Devon L. Hollowood, P. Rooney, Martin Sahlén, Chris A. Collins, Scott T. Kay, D. L. Burke, S. Allam, Robert A. Gruendl, B. Flaugher, C. B. D'Andrea, M. A. G. Maia, Rykoff, E. S., Rozo, E., Hollowood, D., Bermeo-Hernandez, A., Jeltema, T., Mayers, J., Romer, A. K., Rooney, P., Saro, A., Cervantes, C. Vergara, Wechsler, R. H., Wilcox, H., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Benoit-Lévy, A., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Childress, M., Collins, C. A., Cunha, C. E., D'Andrea, C. B., Costa, L. N. Da, Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Evrard, A. E., Finley, D. A., Flaugher, B., Fosalba, P., Frieman, J., Glazebrook, K., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Hilton, M., Honscheid, K., Hoyle, B., James, D. J., Kay, S. T., Kuehn, K., Kuropatkin, N., Lahav, O., Lewis, G. F., Lidman, C., Lima, M., Maia, M. A. G., Mann, R. G., Marshall, J. L., Martini, P., Melchior, P., Miller, C. J., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R., Plazas, A. A., Reil, K., Sahlén, M., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Stott, J. P., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D., Uddin, S., Viana, P. T. P., Vikram, V., Walker, A. R., and Zhang, Y.
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Cosmology and Gravitation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Star (game theory) ,media_common.quotation_subject ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Lambda ,01 natural sciences ,Clusters ,0103 physical sciences ,clusters: general [galaxies] ,Astrophysics::Solar and Stellar Astrophysics ,Deslocamento para o vermelho ,galaxies: clusters: general ,Astronomy and Astrophysics ,Space and Planetary Science ,General ,010303 astronomy & astrophysics ,STFC ,Galaxy cluster ,Astrophysics::Galaxy Astrophysics ,Photometric redshift ,media_common ,QB ,Aglomerados de galaxias ,Physics ,010308 nuclear & particles physics ,Energia escura ,Astrophysics::Instrumentation and Methods for Astrophysics ,RCUK ,Astronomy and Astrophysic ,Galaxies ,Galaxy ,Redshift ,Fotometria astronômica ,South Pole Telescope ,Sky ,astro-ph.CO ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We describe updates to the \redmapper{} algorithm, a photometric red-sequence cluster finder specifically designed for large photometric surveys. The updated algorithm is applied to $150\,\mathrm{deg}^2$ of Science Verification (SV) data from the Dark Energy Survey (DES), and to the Sloan Digital Sky Survey (SDSS) DR8 photometric data set. The DES SV catalog is locally volume limited, and contains 786 clusters with richness $\lambda>20$ (roughly equivalent to $M_{\rm{500c}}\gtrsim10^{14}\,h_{70}^{-1}\,M_{\odot}$) and $0.2, Comment: 21 pages, accepted to ApJS (The Astrophysical Journal Supplement Series, Volume 224, Issue 1, article id. 1, pp. (2016))
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- 2016
48. Cross-correlation of spectroscopic and photometric galaxy surveys: cosmology from lensing and redshift distortions
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Enrique Gaztanaga, Pol Martí, Martin Eriksen, Ramon Miquel, Pablo Fosalba, Francisco J. Castander, Anna Cabré, and Martin Crocce
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Physics ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,Galaxy ,Cosmology ,Redshift ,Redshift-space distortions ,Space and Planetary Science ,0103 physical sciences ,Dark energy ,Baryon acoustic oscillations ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Weak gravitational lensing ,Photometric redshift - Abstract
Cosmological galaxy surveys aim at mapping the largest volumes to test models with techniques such as cluster abundance, cosmic shear correlations or baryon acoustic oscillations (BAO), which are designed to be independent of galaxy bias. Here we explore an alternative route to constrain cosmology: sampling more moderate volumes with the cross-correlation of photometric and spectroscopic surveys. We consider the angular galaxy-galaxy autocorrelation in narrow redshift bins and its combination with different probes of weak gravitational lensing (WL) and redshift space distortions (RSD). Including the cross-correlation of these surveys improves by factors of a few the constraints on both the dark energy equation of state w(z) and the cosmic growth history, parametrized by \gamma. The additional information comes from using many narrow redshift bins and from galaxy bias, which is measured both with WL probes and RSD, breaking degeneracies that are present when using each method separately. We show forecasts for a joint w(z) and \gamma figure of merit using linear scales over a deep (i
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- 2012
49. The difference imaging pipeline for the transient search in the Dark Energy Survey
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M. A. G. Maia, J. J. Thaler, R. Covarrubias, David Goldstein, A. Papadopoulos, Gary Bernstein, P. Martini, Fang Yuan, Flavia Sobreira, R. C. Thomas, C. B. D'Andrea, Robert Connon Smith, S. Allam, Robert A. Gruendl, Francisco J. Castander, Daniel Scolnic, F. B. Abdalla, W. C. Wester, Joshua A. Frieman, David J. James, H. T. Diehl, I. Sevilla-Noarbe, Ryan J. Foley, S. Desai, Daniel Gruen, N. Kuropatkin, J. P. Marriner, Ricardo L. C. Ogando, L. N. da Costa, R. R. Gupta, Tim Eifler, A. A. Plazas, A. Roodman, K. Honscheid, M. J. Marcha, Martin Crocce, C. J. Miller, Ramon Miquel, M. Sako, David J. Brooks, E. Bertin, M. J. Childress, Douglas L. Tucker, G. Tarle, Mark Sullivan, Alistair R. Walker, Kyler Kuehn, Marcelle Soares-Santos, T. M. C. Abbott, M. Carrasco Kind, Richard Kessler, Mathew Smith, Robert C. Nichol, E. J. Sanchez, B. Flaugher, Tianjun Li, A. K. Romer, D. A. Finley, A. Fausti Neto, A. Carnero Rosell, A. Benoit-Lévy, Jennifer L. Marshall, and J. L. Fischer
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Physics ,Cosmology and Gravitation ,010308 nuclear & particles physics ,Pipeline (computing) ,Monte Carlo method ,Subtraction ,FOS: Physical sciences ,RCUK ,Astronomy and Astrophysics ,Astrophysics ,Light curve ,01 natural sciences ,Redshift ,Supernova ,Space and Planetary Science ,0103 physical sciences ,Dark energy ,Variable star ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,STFC ,QB ,astro-ph.IM - Abstract
We describe the operation and performance of the difference imaging pipeline (DiffImg) used to detect transients in deep images from the Dark Energy Survey Supernova program (DES-SN) in its first observing season from 2013 August through 2014 February. DES-SN is a search for transients in which ten 3 deg2 fields are repeatedly observed in the g, r, i, z passbands with a cadence of about 1 week. The observing strategy has been optimized to measure high-quality light curves and redshifts for thousands of Type Ia supernovae (SNe Ia) with the goal of measuring dark energy parameters. The essential DiffImg functions are to align each search image to a deep reference image, do a pixel-by-pixel subtraction, and then examine the subtracted image for significant positive detections of point-source objects. The vast majority of detections are subtraction artifacts, but after selection requirements and image filtering with an automated scanning program, there are ˜130 detections per deg2 per observation in each band, of which only ˜25% are artifacts. Of the ˜7500 transients discovered by DES-SN in its first observing season, each requiring a detection on at least two separate nights, Monte Carlo (MC) simulations predict that 27% are expected to be SNe Ia or core-collapse SNe. Another ˜30% of the transients are artifacts in which a small number of observations satisfy the selection criteria for a single-epoch detection. Spectroscopic analysis shows that most of the remaining transients are AGNs and variable stars. Fake SNe Ia are overlaid onto the images to rigorously evaluate detection efficiencies and to understand the DiffImg performance. The DiffImg efficiency measured with fake SNe agrees well with expectations from a MC simulation that uses analytical calculations of the fluxes and their uncertainties. In our 8 ``shallow'' fields with single-epoch 50% completeness depth ˜23.5, the SN Ia efficiency falls to 1/2 at redshift z ≈ 0.7; in our 2 ``deep'' fields with mag-depth ˜24.5, the efficiency falls to 1/2 at z ≈ 1.1. A remaining performance issue is that the measured fluxes have additional scatter (beyond Poisson fluctuations) that increases with the host galaxy surface brightness at the transient location. This bright-galaxy issue has minimal impact on the SNe Ia program, but it may lower the efficiency for finding fainter transients on bright galaxies.
- Published
- 2015
50. The dark energy camera
- Author
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P. Doel, A. A. Plazas, Kevin Reil, R. H. Schindler, J.-P. Rheault, Douglas L. Tucker, A. Roodman, Armin Karcher, Ricardo L. C. Ogando, L. Beaufore, B. Yanny, G. Gutierrez, R. Schmitt, H. Cease, Marco Bonati, G. Derylo, Katherine Schultz, K. Honscheid, Rebecca A. Bernstein, Curtis Weaverdyck, Robert J. Woods, Eric H. Neilsen, Josh Frieman, Jennifer L. Marshall, R. Flores, M. Jonas, J. Lee, Darren L. DePoy, S.E. Holland, O. Alvarez, Richard G. Kron, Jiangang Hao, John Peoples, H. T. Diehl, Terri Shaw, J. Emes, A. Sypniewski, D. Boprie, Donna Kubik, B. Flaugher, S. E. Kuhlmann, B. Bigelow, Juan Estrada, V. Scarpine, J. M. Cela-Ruiz, Michael Schubnell, R. Angstadt, Cheryl Jackson, David J. James, W. C. Wester, D. A. Finley, J. Rauch, K. Patton, K. Kuehn, Ann Elliott, Alex Drlica-Wagner, N. Palio, A. Lathrop, O. Ballester, F. Munoz, M. Antonik, K. Kuk, D. Huffman, T. M. C. Abbott, J. De Vicente, Ricardo Schmidt, O. Lahav, J. Campa, Michael D. Gladders, Steve Kent, Robert C. Nichol, J. Annis, Mark Kozlovsky, E. J. Sanchez, B. Gregory, G. Wang, Tianjun Li, Steve Chappa, E. Dede, M. G. Watson, C. Cooper, Robert Connon Smith, H. Rogers, Gary Bernstein, Jon J Thaler, Brian Nord, Jamieson Olsen, Natalie A. Roe, C. Tran, Javier Castilla, K. W. Merritt, W. Stuermer, Ramon Miquel, I. Karliner, Francisco J. Castander, G. Martinez, R. Tighe, David J. Brooks, Peter Lewis, G. Tarle, L. N. da Costa, A. Fausti Neto, L. Scott, Laia Cardiel-Sas, S. Serrano, Edward C. Chi, Richard Kessler, Michael Levi, A. Stefanik, E. Suchyta, J. Eiting, Alistair R. Walker, Marcelle Soares-Santos, Scott Holm, P. Schurter, I. Mandrichenko, E. Buckley-Geer, and D. W. Gerdes
- Subjects
Cosmology and Gravitation ,Aperture ,FOS: Physical sciences ,Field of view ,Noise (electronics) ,law.invention ,Telescope ,WNU ,Optics ,surveys ,law ,Shutter ,photometers [instrumentation] ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,STFC ,Physics ,detectors [instrumentation] ,Pixel ,business.industry ,RCUK ,Astronomy and Astrophysics ,observations [cosmology] ,atlases ,Cardinal point ,Space and Planetary Science ,Astrophysics - Instrumentation and Methods for Astrophysics ,business ,Focus (optics) ,catalogs ,astro-ph.IM - Abstract
The Dark Energy Camera is a new imager with a 2.2-degree diameter field of view mounted at the prime focus of the Victor M. Blanco 4-meter telescope on Cerro Tololo near La Serena, Chile. The camera was designed and constructed by the Dark Energy Survey Collaboration, and meets or exceeds the stringent requirements designed for the wide-field and supernova surveys for which the collaboration uses it. The camera consists of a five element optical corrector, seven filters, a shutter with a 60 cm aperture, and a CCD focal plane of 250 micron thick fully-depleted CCDs cooled inside a vacuum Dewar. The 570 Mpixel focal plane comprises 62 2kx4k CCDs for imaging and 12 2kx2k CCDs for guiding and focus. The CCDs have 15 microns x15 microns pixels with a plate scale of 0.263 arc sec per pixel. A hexapod system provides state-of-the-art focus and alignment capability. The camera is read out in 20 seconds with 6-9 electrons readout noise. This paper provides a technical description of the camera's engineering, construction, installation, and current status., Comment: submitted to AJ Corresponding Authors H. T. Diehl (diehl@fnal.gov)
- Published
- 2015
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